Lynn B. Wilson III NASA GSFC Project Scientist Executive ... · 2017 Wind Senior Review Executive Summary Wind 2017 Senior Review Proposal Lynn B. Wilson III NASA GSFC Project Scientist

2017 Wind Senior Review Executive Summary

Wind 2017 Senior Review ProposalLynn B Wilson III

NASA GSFCProject Scientist

Executive SummaryNASA launched the Wind spacecraft in November 1994 to the Earthrsquos L1 Lagrange point as the interplan-

etary component of the Global Geospace Science (GGS) Program within the International Solar TerrestrialPhysics (ISTP) program The spin stabilized spacecraft ndash spin axis aligned with ecliptic south ndash carries eightinstrument suites that provide comprehensive measurements of thermal to solar energetic particles quasi-static fields to high frequency radio waves and γ-rays All instrument suites continue to provide valuablescientific observations completely available to the public (except TGRS now without coolant)

Figure 1 Wind a comprehensive solar wind monitor

The Wind instrument suite provides comprehensive and unique high time resolution (HTR) in-situ solarwind measurements that enable the investigation of wave-particle interactions Wind is the only near-Earthspacecraft equipped with radio waves instrumentation Wind has made numerous independent discoveriessince the last Senior Review from kinetic effects of solar wind reconnection and plasmas to solar cycleseasonal variations Wind remains very active as evidenced by the over 600 refereed publications in2015-2017 (over 4300 refereed publications since launch listed on the Wind project Web pagehttpswindnasagov) 13 doctoral and 3 Masters degrees (86 total graduate degrees since 1994) and16 currently in progress The new results span all three heliophysics research objectives as described in the2014 Science Plan for NASArsquos Science Mission Directorate The Wind science data products are publiclyserved directly from the instrument team sites and CDAWeb with a single project webpage containing linksto and descriptions of the large number of Wind data products Wind is also an active participant in thedevelopment of the Virtual Heliophysics Observatory (VHO) that allows for more complex queries thanCDAWeb

Even though Wind is gt22 years old the spacecraft is still in good health Wind continues to remain anactive mission as evidenced by the gt1825000 data access requests registered by CDAWeb for Wind andOMNI data (which largely relies upon Wind and ACE measurements) between Jan 1 2015 and Jan 1 2017Because of its longevity Wind observations will allow researchers to compare long-term variations in solarwind properties solar wind transients and micron-sized dust fluxes for solar cycles 22ndash24 without needingto compensate for changing instrumentation and calibration Furthermore new Wind data produced sincethe last Senior Review will provide unprecedentedly accurate and high time energy and angularresolution measurements of the near-Earth solar wind

Wind continues to remain a relevant mission as evidenced by recent press releases and high impact pub-lications (ie 12 in Nature and 7 in Phys Rev Lett since 2015) for instance at

1 of 44

2017 Wind Senior Review

httpwwwnaturecomarticlessrep08080httpswwwnasagovfeaturegoddard2016nasa-finds-unusual-origins-of-high-energy-electrons

Wind has also contributed critically to multi-mission studies as part of the Heliophysics System Obser-vatory (HSO) With its ample fuel reserves sufficient for gt50 years Wind will continue to provide accuratesolar wind input for magnetospheric studies (supporting MMS THEMIS and Van Allen Probes) and serveas the 1 AU reference point for outer heliospheric (eg Voyager MAVEN JUNO) investigations in additionto providing critical support for other NASA missions (eg STEREO ACE DSCOVR etc) Moreovernew Wind results will continue to improve theories of solar wind heating acceleration and energetic par-ticle processes to focus the science objectives of future missions (eg Solar Probe Plus and Solar Orbiter)Once these new missions are launched Wind will provide critical measurements to complement theobservations made by Solar Probe Plus and Solar Orbiter which will enable researchers torelate the solar wind at 1 AU to its coronal sourse and compare radio burst power with sourcelocations

Rationale for Continuing the Wind Missionbull Wind continues to provide unique robust and high resolution solar wind measurementsbull Wind will serve as the 1 AU reference for Solar Probe Plus and Solar Orbiterbull Wind aids in cross-calibration efforts for the DSCOVR and ACE missionsbull Wind and ACE are complementary not identical rArr both are needed for complete 1 AU observationsbull Wind still has redundant systems instruments and enough fuel for gt50 yearsbull Wind rsquos high scientific productivity rarr significant discoveries in all three SMD research objectives

Table of ContentsExecutive Summary 11 Science and Science Implementation 3

11 Historical Background 312 Current Status 313 Wind rsquos Unique Capabilities 314 Heliophysics System Observatory 4

2 Prior Prioritized Science Goals 621 PSG 1 Two Full Solar Cycles 622 PSG 2 Solar Wind Structures 723 PSG 3 Kinetic Physics 924 PSG 4 Dust Science 1325 Noteworthy Studies 14

3 New Prioritized Science Goals 1431 Field-Particle Studies 1532 Unusual Solar Cycle 1733 Particle Acceleration 1834 Long-Term Dust Science 19

4 Wind in the Heliophysics System Observatory 1941 Wind and ACE DSCOVR STEREO and MAVEN 1942 Wind and Solar Probe Plus and Solar Orbiter 2043 Wind and IBEX and Voyager 2144 Wind and Van Allen Probes MMS THEMIS and Cluster 2145 Solar and Astrophysics 2146 Wind CCMC and CDAW Data Center 22

5 Technical Implementation 2351 Spacecraft Health 2352 Instrument Status 2453 Science Team 2454 Ground Operations 25

6 In-Guide Budget 2661 Mission Operations 2662 Data Production and Accessibility 27

References 27A Mission Archive Plan 31Acronyms and Initialisms 39Budget Spreadsheet 44

2 of 44

2017 Wind Senior Review Science and Science Implementation

1 Science and Implementation11 Historical Background

The Wind spacecraft was launched in Novem-ber 1994 as the interplanetary component of theGlobal Geospace Science (GGS) Program withinISTP Wind rsquos original purpose was (1) to make ac-curate in-situ measurements of interplanetary con-ditions upstream of the magnetosphere to comple-ment measurements made in the magnetosphere byPolar and Geotail and (2) to remotely sense inter-planetary disturbances for possible future predictivepurposes The instruments were therefore designedto make highly accurate solar wind measurements

Prior to May 2004 Wind performed a series oforbital maneuvers (see Figure 2) that led to sim67petal orbits through the magnetosphere out of theecliptic plane lunar rolls in April and May of 1999four east-west prograde 13ndashLissajous orbits reachingamp300 RE along the plusmnY-GSE direction between Au-gust 2000 and June 2002 and an excursion to theL2 Lagrange point from November 2003 to February2004 (ie gt220 RE downstream of Earth and sim500RE downstream of ACE) In May 2004 Wind movedto L1 where it has remained and will stay for theforeseeable future Note that Wind rsquos L1 orbit hasa plusmnY-GSE displacement about the sun-Earth line ofsim100 RE much larger than ACE or DSCOVR

12 Current StatusThe Wind spacecraft continues to operate in good

health In 2000 the team successfully reconfiguredthe communications system to enhance the teleme-try margin Reliance on a single digital tape recorder(with two tape units TUA and TUB) since 1997has never hampered operations and the team tookmeasures to minimize its use in order to extend taperecorder life as long as possible

Seven of the eight Wind instruments including allof the particles and fields instruments remain largelyor fully operational The EPACT high energy par-ticle and SMS solar wind composition instrumentssuffered some degradation but both continue to pro-vide valuable measurements The SWE electron in-strument required some reconfiguration to maintainits capabilities The TGRS γ-ray detector was beenturned off as planned due to it no longer having suf-ficient coolant to operate For technical details seeSection 52

In May 2014 the 3DP instrument (specificallyPESA Low) suffered an anomaly that only affectedthe telemetry house keeping data The science dataremained unaffected and continues to return the high-est resolution velocity moments of the solar wind ofany near-Earth spacecraft All the other instruments

operate nominally Thus the net loss in capabilityremains minimal and the Wind instruments continueto provide definitive and continuous measurements ofthe solar wind

On Oct 27 2014 at 215938 GMT the Wind com-mand and attitude processor (CAP) suffered two sin-gle event upsets (SEUs) The redundant nature ofthe Wind spacecraft bus allowed the flight operationsteam (FOT) to successfully switch to a second CAPCAP2 The FOT began the recovery of CAP1 onJan 21 2015 and finished Jan 30 2015 Thus theWind spacecraft was fully recovered at sim1750 UTCon Jan 30 2015 For more details please see Section51

On April 11 2016 one of the two tape units (TUA)began experiencing issues related to the readwritehead causing simfew percent data loss per day Theflight operations team successfully switched the pri-mary record unit to TUB on May 6 2016 to extendthe life of TUA and reduce data loss Wind con-tinues to average gt98 data recovery rates and theTUB status is fully operational

In conclusion Wind is operationally healthy andcontinues to maintain a large fuel reserve capable ofsustaining the spacecraft at L1 for gt50 years

13 Wind rsquos Unique CapabilitiesWind rsquos complement of instruments was optimized

for studies of solar wind plasma interplanetary mag-netic field radio and plasma waves and of low energyparticles The instrument suite is not equivalent tothat of ACE rather the two missions complementeach other ACE ndash launched sim3 years after Windndash focuses on the detailed investigation of high en-ergy particles for which Wind has more limited capa-bilities Several of Wind rsquos solar wind suprathermalparticle and especially radio and plasma wave instru-ments are unique Wind rsquos instrument capabilities aresummarized in Table 1 and are compared to ACE andSTEREO Wind is unparalleled for low energyparticle and radio wave observations of the so-lar wind by near-Earth spacecraft A more de-tailed discussion of Wind rsquos unique capabilities followsbelow

Collaborating with STEREO WindWAVES pro-vides an essential third vantage point along the Sun-Earth line allowing the unambiguous localization ofinner heliospheric radio sources and the determina-tion of their corresponding beam patterns More im-portantly Wind is the only spacecraft at L1 thatcan observe the upper hybrid line (or plasma line)which provides the most accurate and only unam-biguous measurement of the total electron density inthe solar wind Thus the density ndash normally ob-tained as a moment or fit of the velocity distribution

3 of 44

-100-200 0 200100 300-300Xgse [Re]

Wind Orbit 2000-08-19 to 2015-12-312000-08-19 to 2001-09-09

2001-09-10 to 2001-12-08

2001-12-09 to 2002-07-28

e] -100

-100-200 0 200100 300-300Xgse [Re]

Wind Orbit 1994-11-01 to 2000-08-18

1994-11-01 to 1996-05-13

1996-05-14 to 1996-08-11

1994-08-12 to 1997-01-09

1997-01-10 to 1997-05-29

1997-05-30 to 1997-10-31

1997-11-01 to 1998-06-19

1998-06-20 to 1999-05-12

1999-05-13 to 1999-08-12

1999-08-13 to 2000-08-18

2002-07-29 to 2002-12-03

2002-12-04 to 2003-06-28

2003-06-29 to 2004-04-28

2004-04-29 to 2015-12-31

Figure 2 Orbital trajectories of the Wind spacecraft in the GSE XY plane from 1 November 1994 to 31 December2015 Colors denote time ranges as indicated The dashed black circle indicates the Moonrsquos orbit (Adapted fromFigure 1 in Malaspina and Wilson III [2016])

function from particle instruments like SWE and 3DPndash can be accurately and independently derived fromthe WAVES instrument The WAVES instrumentprovides the only method for an independentin-flight and absolute calibration for particleinstruments for spacecraft near L1

Wind is unparalleled in its capacity for high timeresolution (HTR) measurements of quasi-static mag-netic fields (MFI instrument) and thermal solar windelectrons (3DP) Though STEREOSWEA has ahigher cadence in burst mode the low energy (60eV) electrons cannot be measured by the detector[eg Fedorov et al 2011] causing Wind3DP to havethe highest time resolution measurements of thermalelectrons WindMFI offers continuous coverage ofthe quasi-static magnetic fields at sim11 samples persecond (sps) over the entire mission (sim22 sps whenWind was within 100 RE of Earth) still the highestsample rate of science-quality continuous solar windmeasurements

WindSTICS is unique among currently opera-tional spacecraft as it is the only sensor in space fullydedicated to providing measurements of heavy ionsfor an energy range spanning sim62ndash2231 keVamuAs STICS is a time-of-flight mass spectrometer itcan differentiate many minor ionic species and lookat their characteristics in the suprathermal energyrange to better understand their origin In additionWindLEMT provides high energy particle data overa range of energies not covered by ACE (ie sim1ndash10MeVamu)

The WindWAVES instrument can also be usedfor solar energetic particle (SEP) studies For in-

stance Malandraki et al [2012] and Agueda et al[2014] made detailed comparisons of the injectiontime histories of selected SEP events as derived fromthe modeling of the interplanetary transport of elec-trons and protons with electromagnetic emissionsparticularly with decametric-hectometric (DH) typeIII radio bursts A close correspondence was foundand this underlines the usefulness of type III burstsas a constraint of energetic particle release to inter-planetary space Wind is still the only near-Earthspacecraft which can measure both the electromag-netic and particle signatures of SEP events ThusWind rsquos distinct capacities make it as a valu-able asset to the Heliophysics community andan essential component in the HSO

14 Heliophysics System ObservatoryWind plays an active role in the Heliophysics Sys-

tem Observatory (HSO) Wind achieved many ofits recent scientific discoveries in collaboration withother spacecraft as described in more detail in Section4 Participation in the HSO enables more such col-laborative studies in the future by providing a dataenvironment where such comparisons can be read-ily performed As the Heliophysics Data Policy out-lines this data environment requires the presence ofin-depth metadata for each data product based ona uniform standard (the SPASE dictionary) It alsoenvisions the eventual connection of the distributeddata repositories by a number of virtual observatoriesenabling the location and downloading of the desireddata Wind plays a leadership role in the deploymentof the Virtual Heliospheric Observatory (VHO) theheliospheric portion of this environment and the gen-

4 of 44

Table 1 The measurement capabilities of Wind compared to STEREO and ACEType Wind STEREO ACE Comments for Wind

DC Magnetic MFI MAG MAG highest time resolutionField sim11 spsa sim8 sps (sim32 sps burst) sim6 sps for continuous coverage

unique large antenna lengthRadio WAVES SWAVES NA allows for measurement of localWaves sim4kHzndash14MHz sim25kHzndash16MHz plasma frequency rarr electron

densitysearch coil and long antenna

Time Domain TDS TDS NA rarr better calibration andWaveforms sim19ndash120kspsb sim78ndash250ksps more sensitive

Thermal 3DPc highest time angular andIons SWE PLASTIC SWEPAM energy resolution robust and

(Moments) sim92 s sim60 s sim64 s redundant operates during solarstorms

Thermal 3DP PLASTIC SWEPAM highest time angular andIons (DFsd) sim24 se NA NA energy resolution

Thermal 3DP (sim3 s) SWEAf SWEPAM highest time resolutionElectrons SWE (sim9 s) (sim2 s) (sim128 s) for full 4π coverage

(Moments) at low energyThermal 3DP SWEA SWEPAMElectrons sim3 s sim2 s NA [same as above]

Solar Wind SMSSTICS PLASTIC SWICS onlyComposition 1leZle56 1leZle56 1leZle30 observations

sim03ndash230keVQ sim03ndash80keVQ sim05ndash100keVQ gt 100 keVQMass SMSMASS NA SWIMS comparable to

Spectrometry 1leZle28 NA 2leZle30 ACE in bothsim05ndash12keVQ NA sim05ndash20keVQ charge and energy

Low SWEAg SWEPAM full 3D measurementsEnergy 3DP SEPTh EPAM from a few eV

Electrons sim3eVndash500keV STEi sim3eVndash400keV to sim500 keVLow SWEPAMj measurements of solar

Energy 3DP SEPT EPAMk wind thermal coreIons sim3eVndash7MeV sim60keVndash7MeV ULEISl to lower energiesHigh SITm SIS robust high geometry factor

Energy EPACTLEMT LETn CRIS unique directional observationsParticles sim004ndash50MeVn HETo sim10ndash600MeVn and energy range

a sim22 samples per second when inside 100 RE b kilosamples per secondc moments sim3s distributions sim24s burst sim3s d DF = velocity distribution function e sim3s in burst modef nothing below sim60eV g sim60ndash3000eV h sim2ndash100keV 48 telescopes contaminated i sim30ndash400keVj sim260eVndash35keV k sim46ndash4800keV l sim45keVnndash2MeVn m sim003ndash5MeVn n sim2ndash60MeVn o sim1ndash170MeVn

eration of the corresponding metadataThe Living With a Star (LWS) program seeks to

better understand the Sun-Earth connected systemwith the aim of developing reliable space weatherforecasting capabilities The program architectureplan calls for a near-Earth solar wind monitor to con-nect the solar (SDO) and inner heliospheric (eg So-lar Probe Plus and Solar Orbiter) observations withgeomagnetic ones (eg Van Allen Probes) How-ever NASA has no plans for a new solar wind

and solar energetic particle (SEP) monitoringmission until at least 2024 Rather NASA as-sumes that Wind ACE or both will survive into the2017ndash2022 time frame DSCOVR has only limitedmeasurement capabilities (Faraday Cup and magne-tometer) and fuel only for about five years leavingWind and ACE still as the primary near-Earth as-sets during the primary phase of the Solar Probe Plusand Solar Orbiter missions The lowest risk optionto satisfy the near-Earth solar wind monitoring re-

5 of 44

2017 Wind Senior Review Prior Prioritized Science Goals

quirement of LWS is to sustain both Wind and ACEndash either of which can satisfy the LWS measurementrequirements ndash because both are well past their primemissions and design lifetimes Again note that Windand ACE are not duplicate spacecraft but ratherserve complementary roles Thus the most prudentcourse of action involves preserving both spacecraft

In the following we discuss our progress on the pre-vious set of Prioritized Science Goals (PSGs)

2 Previous PSGs

Prior Prioritized Science Goals1 Long-term variations Two Full Solar Cycles2 Solar Wind Structures3 Kinetic Signatures of Heating and Acceleration4 Dust science

The Wind mission is operating on a minimal bud-get that does not allow for the dedicated support ofany in-depth focused scientific research The fundingis applied to the operation of the spacecraft and thecollection and validation of high quality solar windmeasurements As part of the instrument data vali-dation process several significant scientific discover-ies have been made in recent years as outlined in thefollowing sections Most detailed scientific researchusing Wind data is primarily supported under theROSES GI and SRampT programs In the followingsections we outline several Wind results relating toour past focused science research topics

21 PSG 1 Two Full Solar Cycles

SSN STs

1995 2000 2005 2010 2015

Figure 3 Distribution of yearly numbers of STsobserved by Wind (green trace) from 1995ndash2014 Thesunspot numbers (SSN) are shown in black The toppanel gives a histogram of ICMEs (yellow) frompublished tabulations [eg Richardson and Cane 2010](Adapted from Figure 11 in Yu et al [2016])

Wind was launched at the tail end of solar cycle(SC) 22 (ie March 1986 to May 1996) and has pro-vided continuous measurements through all of SC23

(ie June 1996 to December 2008) and the currentextent of SC24 (ie January 2009 to Present) [Hath-away 2015] in its gt22 years of operation ThusWind has at least some solar wind data from threedifferent solar cycles The time range included forthis Senior Review will likely cover the rest of SC24and may include the beginning of SC25 In this sec-tion we discuss some recent progress towards under-standing the dependence of long-term phenomena onthe solar cycle

One of the many phenomena thought to be depen-dent upon the SC are solar transients eg coronalmass ejections or CMEs Small transients (STs) ndashmagnetic field configurations whose passage at Earthmay last from a few tens of minutes to a few hours ndashhave gained recent interest due to their relationshipwith the slow solar wind Yu et al [2016] presenteda statistical study of STs observed by Wind andSTEREO for the 20 year period 1995ndash2014 (STEREOonly from 2006 onward)

Table 2 ICME Parameters over 3 Solar Cycles(Adapted from Nieves-Chinchilla et al [2017])

Parameter SC22a SC23 SC24

of Events 13 169 119

of Daysb sim577 sim4597 sim2556c

of EventsYeard sim8 sim13 sim17

〈B〉e [nT] NA sim12 sim10

〈V sw〉f [kms] NA sim459 sim381

〈np〉g [cmminus3] NA sim73 sim77

Parameter Mini Maxj Meank

|B| [nT] sim3 sim33 sim11

|V sw| [kms] sim270 sim968 sim433

a SC = solar cycle b of Julian days of Wind cov-

erage c up to Dec 31 2015 or sim7730 total daysd 365 day years e average over SC coverage f solar

wind bulk flow speed g proton number densityh minimum of all events i maximum of all eventsj average of all events

Figure 3 presents the long-term (including datafrom three SCs) occurrence frequency of STs vs theSSN (black line) and ICMEs (yellow histogram) Aclear anti-correlation with SSN is evident The STnumber peaks in 2009 a year of a deep solar mini-mum This trend is opposite to that of large ICMEsSimilar results were obtained by the STEREO probesfar from the Sun-Earth line The plot raises severalquestions in light of the recent ldquoweakrdquo SC

In addition to STs another phenomenon whosestudy benefits greatly from three SCs of data isICMEs ICMEs are manifestations of magnetizedplasma moving from the Sun throughout the helio-

6 of 44

sphere and also main triggers of geomagnetic activityThese solar transient structures are often character-ized by a well organized magnetic structure embeddedwithin the ICME known as Magnetic Clouds (MCs)Developing a reliable space weather forecasting sys-tem requires the simultaneous observation of the ve-locity size plasma density and magnetic topology ofICMEs

Nieves-Chinchilla et al [2017] performed a statis-tical study of ICMEs observed by Wind from 1995ndash2015 Table 2 summarizes some of the SC propertiesof magnetic obstacles from the Wind ICME catalogue(httpswindgsfcnasagovICMEindexphp)

tion (

minus4 P

1995 1996 1997 1998 1999 2000 2001 2002 2003 2004 2005 2006 2007 2008 2009 2010 2011 2012 2013 2014 2015year of solar cycle

Cycle 22 Cycle 23 Cycle 24

Figure 4 Summary of ICME statistics by year of theSC from the Wind ICME catalogue for SC22 (green)SC23 (red) and SC24 (blue) The panels shown areyearly averages of the following (in order fromtop-to-bottom) of ICMEs with embedded flux-ropesflux-rope duration [hrs] dynamic pressure [Pa] solarwind bulk flow speed [kms] flux-rope expansion speed[kms] and magnetic field magnitude (Adapted fromNieves-Chinchilla et al [2017])

Figure 4 compares the yearly averages of ICMEsfrom the Wind ICME catalogue for SC23 (red) andSC24 (blue) The expansion speed is defined as one-half the difference between solar wind bulk speed atthe start and end time of the flux-rope embeddedwithin the ICME The maximum number of ICMEsappears earlier in SC23 than SC24 which exhibitsa ldquobell shapedrdquo profile with a maximum in year 4(ie 2012) The average yearly rate of events is 14for both SC23 and SC24 (eg see Table 2) The dy-namic pressure resembles a bimodal distribution forSC23 but is less well pronounced for SC24 The solarwind speed and magnetic field magnitudes howevershow little solar cycle dependence However for both

parameters SC24 shows slightly weaker values thanSC23

These studies highlight the SC dependence of so-lar wind transient structures Wind -related work hasalso found that SEPs and solar flares depend uponthe SC [Dierckxsens et al 2015] Further the pres-ence of continuous coverage can improve the accuracyof long-term predictive models of solar cycles [egZachilas and Gkana 2015] These studies provideillustrative examples of the importance of con-tinuous coverage by a single spacecraft overlong durations like Wind without which suchinvestigations would suffer

22 PSG 2 Solar Wind StructuresSmall transients (STs) ndash magnetic field configura-

tions whose passage at Earth may last from a few tensof minutes to a few hours ndash may play a role in thedevelopment of the slow solar wind As mentionedin the previous section an extensive statistical studyof the occurrence and properties of small solar windtransients (STs) was presented by Yu et al [2016]It was based on Wind and STEREO data for the 20year period 1995ndash2014 The authors examined thedependence of ST occurrence frequency in (i) solarcycle phase and (ii) solar wind speed during the STsThey define the latter by taking the average speed ofthe STs since these transients tend to convect withthe surrounding flow

Figure 5 shows the distribution of solar wind speedsfor STs as observed by Wind and both STEREOspacecraft The huge majority of STs lie in the slowwind The velocity distribution peaks in the sim300ndash400 kms velocity bin for all three spacecraft Thisvelocity dependence is much stronger than that ofthe solar cycle For example we contrast the ST oc-currence in 2009 with that of 2003 Roughly 27of 2003 corresponded to slow solar wind while sim89of 2009 was slow solar wind (ie sim33 times higher)Rather than observing sim3 times as many STs in 2009as in 2003 the authors reported sim64 times as manyThus the authors argue that the STs may be an im-portant constituent of the slow solar wind

The Wind mission has been providing insitu plasma energetic particles and mag-netic field observations since late 1994 TheWind team maintains an online catalogue(httpswindgsfcnasagovICMEindexphp) ofEarth-directed ICME events with well organizedmagnetic topology ndash known as Magnetic Clouds(MCs) ndash observed by Wind from 1995ndash2015 MCs aredefined here as the interval within an ICME wherethe magnetic pressure dominates over the plasmapressure (ie sub-unity plasma β) with an organizedmagnetic topology similar to the conceptual picture

7 of 44

200~250

250~300

300~350

350~400

400~450

450~500

500~550

550~600

600~650

650~700

700~750

Velocity)(kms))

Velocity)Distribu4on)of)STs)

Wind STA STB

Figure 5 Velocity distribution of STs as measured byWind from 1995ndash2014 and both STEREO spacecraftfrom 2006ndash2014 A vertical line has been drawn at V sim450 kms separating slow from fast winds (Adaptedfrom Figure 12 in Yu et al [2016])

of a heliospheric flux-rope (FR) The main webpageof the ICME catalogue presents links to the yearsincluded in the catalogue

The following are included for each eventICME start and end times magnetic obsta-cle start and end times a link to the as-sociated interplanetary (IP) shock (ie athttpwwwcfaharvardedushockswi data) ifpresent the magnetic obstacle classification meanmagnetic field solar wind bulk velocity and theexpansion velocity [Nieves-Chinchilla et al 2017]The magnetic obstacle embedded within the ICMEis defined as a FR ndash traditionally called magneticclouds or MCs ndash for events with at least one mag-netic rotation and ejecta (E) when no clear magnetictopology is detected Every event also includes alink to a plot of the data for the event and a linkto the integrated Space Weather Analysis system(iSWA httpsiswagsfcnasagov) which presentsan overview of the state of the heliosphere duringthe ICME propagation to the Earth

Figure 6 shows an example ICME observed byWind on January 1 2010 The EEP parameter(ie last panel) was introduced by Nieves-Chinchillaet al [2016] to quantify the bi-directionally of theelectrons The EPP is the ratio of the average elec-tron intensity of the parallel (ie 0ndash18) and anti-parallel (ie 162ndash180) pitch-angles to the perpen-dicular (ie 78ndash96) pitch-angles The inner-twodashed lines (ie from 2010-01-02002400 UT to2010-01-03083800 UT) enclose the flux-rope (ieMC) defined by an increase in magnetic field magni-tude rotation in Bz and low βp The first dashedline (ie at 2010-01-01220400 UT) shows the startof an IP shock followed by the sheath region It canbe seen that the EPP goes to zero at the IP shockand remains there until roughly the second half ofthe flux-rope The bi-directional electron flows dur-ing the second half suggest a connection of both ends

Figure 6 In situ data from the MFI and SWEinstruments onboard the Wind spacecraft on January 12010 The panels shown are the following (in order fromtop-to-bottom) magnetic field magnitude magnetic fieldcomponents (GSE) proton number density protonthermal speed proton beta βp solar bulk flow speed andthe Electron Pitch-angle distribution (PAD) Parameter(EPP) for 116 and 290 eV electrons The vertical linesshow the interval of the ICME front and flux-ropeboundaries (Adapted from Figure 5 in Nieves-Chinchillaet al [2016])

of the field line to the sunOur current understanding of the magnetic field

topology structure global morphology and the ef-fect of the evolution of ICMEs is still limited Thegt22 years of continuous Wind observations providean opportunity to examine the effects of the ICMEexpansion distortion or interaction with ambient so-lar wind To study the effect ICME expansion ontheir evolution Nieves-Chinchilla et al [2017] defineda Distortion Parameter (DiP) ndash the amount of asym-metry of the magnetic field strength ndash and comparedit to the ICME expansion speed (V exp)

Figure 7 (top) shows the range of DiPs vs V expRegions with V exp lt(gt) 0 correspond to a contract-ing(expanding) ICME The DiP parameter range isfrom 00ndash10 A DiP lt 05 implies a magnetic fieldcompression occurs closer to the spacecraftrsquos first en-counter with the ICME (ie ICME start time) ADiP gt 05 implies the magnetic field compression oc-curs closer to the ICME end time One would expectto have more compression closer to the ICME starttime (ie decreasing DiP lt 05) as V exp increases forexpanding ICMEs An examination of Figure 7 showsthat the events do not follow the expected relation-

8 of 44

minus100 minus50 0 50 100Vexp(kms)

IPCycle 22

Cycle 23

Cycle 24

Figure 7 Top Distortion Parameter (DiP) is shownversus the flux-rope expansion velocity (V exp) The V exp

interval goes from -100 kms to 100 kms The negativevalue of the expansion velocity represent thecompression DiP interval goes from 0 to 1 withsymmetry profile at DiP = 05 magnetic field strengthcompression in the front with DiP lt 05 and magneticfield compression in the back with DIP gt 05 BottomSchematic cartoon illustrating the differences in flux-ropeshapetrajectory for the four quadrants labeled in the topfigure (Adapted from Nieves-Chinchilla et al [2017])

ship between the Vexp and DiP Instead one finds anhomogeneous spread

Figure 7 (bottom) provides a cartoon representa-tion of the possible magnetic field configurations as-sociated with each quadrant in Figure 7 (top) Avisual analysis of individual quadrants (ie A1 A2A3 A4) suggests that the discrepancy could be af-fected by expansion (A1) or also by distortion (A4)curvature (A2) or interaction with the solar wind orother transients (A3) Thus the preliminary resultssuggest all effects may play a role in causing the dif-ference between the expected and observed results

Wind rsquos large database of STs and ICMEs has pro-vided us with a large enough number of events to per-form significant statistical studies on both the generalproperties and SC dependence Wind -related workhas given us evidence that ICMEs exhibit evidenceof distortion curvature and effects due to interac-tion with the solar wind or other transients It isonly because of large statistics due to the long-term continuous coverage of Wind that re-

searchers have been able to examine and beginto understand the evolution of the solar windtransients responsible for the most dramaticgeoaffective space weather events

23 PSG 3 Kinetic PhysicsIn the following section we highlight new results of

kinetic signatures of heating and acceleration usingWind As will be clear from the length of this sectioncompared to the other prior PSGs Wind rsquos uniqueinstrument suites allow for a broad range of kineticstudies

One of the major goals of Wind EPACT-LEMTwas to extend measurements of element abundancesin solar energetic particle (SEP) events throughoutthe periodic table LEMT resolves individual ele-ments up to Z = 26 (Fe) and groups similar similar-Z elements together for higher Z up to Z = 82 (Pb)However in small impulsive events these observationshave revealed a strong power-law enhancement rela-tive to coronal abundances that rises by a factor ofsim1000 from He to Pb as a function of the mass-to-charge ratio AQ as seen in Figure 8

Figure 8 The mean element enhancement in impulsiveSEP events (relative to coronal abundances) is shown vsAQ at 25ndash32 MK where values are taken from theshaded band in Figure 9 The power of the fitted lineshown is 364 plusmn 015 (Adapted from Figure 14 inReames [2015])

The pattern of abundances in Figure 8 is drivenby ionization states Q that only occur at the plasmatemperatures found in solar active regions For exam-ple in solar active regions C is fully ionized like Heand thus un-enhanced while the enhancement of Neexceeds that of Mg and Si etc Individual impulsive

9 of 44

SEP events are strongly bound to this thermal region[Reames et al 2015] These enhancements are be-lieved to result from islands of magnetic reconnection[eg Reames 2016abc and references therein] thatoccur in solar jets reconnecting with open magnetic-field lines where ions easily escape A similar processin flares leads mainly to heating since the acceleratedions are trapped on closed loops

Figure 9 The left panel shows enhancements inelement abundances seen during the large gradual eventof 2000 November 9 The right panel shows AQ vs Tfor various elements The shaded region shows solaractive-region temperatures The groupings ofenhancements match those in AQ near 1 MK (Adaptedfrom Figure 3 in Reames [2016a]) (Reames 2016a b c)

It has been known for many years that power-lawenhancements can also occur in large gradual SEPevents involving acceleration at CME-driven shockwaves Here either enhancements or suppressionscan result from AQ-dependent scattering duringtransport often both occur in a single event Reames[2016a] and Reames [2016b] found that these power-law dependences can also be used to measure sourceplasma temperatures as shown in Figure 9 Here ob-served enhancements in an event on the left are com-pared with the theoretical values of AQ vs T on theright For this event the best fit can be shown to oc-cur at a temperature near 1 MK an ambient coronaltemperature Note that here C N and O are en-hanced more like Ne than He and Si and S havemoved up near Ar and Ca This pattern is quiteunlike that found for the higher-temperature activeregion shown as shaded

In a study of 45 large gradual events [Reames2016a] sim70 had source plasma temperatures ofthe ambient corona (lt16 MK) while sim25 hadactive-region temperatures (25ndash32 MK) This im-

plies that in sim25 of the events the shock wavessweep across active regions and re-accelerated someresidual suprathermal ions from earlier enhanced im-pulsive SEP events diluted by some of the localplasma

Source temperature variations explain many of thesubtle event-to-event abundance variations and com-parisons of impulsive and gradual events at similartemperatures suggest that the shocks are averagingover many small impulsive events that must takeplace almost continuously in active regions [Reames2016b] In the process a new way to measure ioniza-tion states at the point of acceleration was derivedunmodified by traversal of material afterward this isespecially important for impulsive SEP events thatoccur fairly low in the corona These new Windresults are finally helping us to understand thephysics of the energetic particle enhancementsoriginally observed over 30 years ago

-4 -3 -2 -1 0 1

βminusβperp2

ρs|∆

ρv2 A

0[PDF]

Figure 10 2D histogram of solar wind parametersrelevant to the firehose instability The x-axis representsthe total pressure anisotropy of all species and the y-axisrepresents the drifts between all species The black linemarks the long-wavelength firehose threshold with thedata constrained to the stable side Two populations canbe seen corresponding to the presence or absence ofproton beams Adapted from Figure 2 in Chen et al[2016]

In recent years Wind has revealed to us the roleplayed by various plasma instabilities in control-ling the bulk solar wind parameters In particu-lar the firehose and mirror instabilities have beenshown to constrain the plasma beta and temperatureanisotropy of each particle species Chen et al [2016]combined the newly calibrated Wind3DP electrondata set and the newly fitted WindSWE ion dataset (with proton beams) to examine these instabili-ties in a full multi-species context for the first time

Using the theoretical long-wavelength firehose con-dition it was found that the anisotropy and drifts

10 of 44

windowed Fourier spectra of the Bz GSE time series (Bz is thecomponent used in the audio) and the reduced magnetichelicity of the magnetic field vector ms

B t e dt1

22ˆ ( ) ( )ograve= p w

P B B 3ij i jˆ ˆ ( )=

2 Im 4m

i j ij

( ) ( )aring

where Pij are the elements of the reduced power spectral tensorIm() is the imaginary part of the tensor and subscripts i and jdefine the components of the vector We have used a windowofT=2048 samples equivalent to 184 s for the Fouriertransform We smooth the resulting power spectral tensorelements by taking the mean over a 10 fractional windowabout each frequency f f f11 11lt lt acute this removesmuch of the high-frequency variability of the spectrum For thepurpose of plotting as time-frequency spectrograms we theninterpolate the smoothed spectra onto a logarithmically spacedfrequency scale Examples of the original and smoothed spectracan be seen in Figure 3 discussed below and give anindication of the effect of the smoothing and interpolationprocess We also note that because the field in the intervalcontaining the waves is radial the magnetic helicity ms containsthe entire helicity of the magnetic field waves with the othertwo components of the helicity being approximately zero

The wave activity can be seen as a band of increasedamplitude in the Fourier spectra and strong helicity signals inthe frequency range f01 05 Hzlt lt in the spacecraft framebetween DOY 30945 and 30985 in Figure 1 The black line ineach of the bottom two panels of Figure 1 shows a roughestimate of the Doppler-shifted proton gyrofrequency fsc

- in the

frame of the spacecraft

1 5p p

sw swmiddot ( )⎛⎝⎜

⎞⎠⎟p p

raquoW

for a wave propagating parallel ( )+ or antiparallel ( )- to thelocal mean magnetic field with phase speed equal to the Alfveacutenspeed VA (Jian et al 2009) We have purposefully not used amore precise dispersion relation to solve for fsc because theprecise direction and magnitude of k cannot be calculated withcertainty directly from the data and the error in the velocity andchanging magnetic field direction make the uncertainty in theresult large The resonant activity is at a slightly lowerfrequency than fsc

-meaning that the wave either has a lowerfrequency has a higher phase speed or is propagating at aslightly oblique angle to the background magnetic field in theplasma frame This is consistent with previous results from Jianet al (2009 2010 2014)The SWE reduced velocity distribution functions measured

at the same time as the magnetic field are fitted to two bi-Maxwellian velocity distributions one for the core of theproton distribution and one for a suprathermal proton beamcomponent This fit is used to calculate velocity densitytemperature and temperature anisotropy relative to the localmagnetic field direction for each population An example of afield-parallel slice of a fitted distribution is shown in the leftpanel of Figure 2 The density radial velocity and temperatureanisotropy of these two fits are plotted in the first second andthird panels on the right side of Figure 2 respectively Thefourth panel shows the drift of the beam component away fromthe Sun relative to the core along the magnetic field directionnormalized by the local Alfveacuten speed This speed is used tocalculate the kinetic energy density of the beam relative to thecore in Alfveacuten-normalized units in the fifth panel The bi-Maxwellian fit of the SWE distribution functions shows that atthe same time as the MFI data show high-amplitude waves inthe magnetic field the density and kinetic energy of the beamincrease

Figure 1 Time-series plots ofthe observed magnetic field components (top panel)magnetic field angles (second panel)Fourier power spectrum of the Bz component(third panel)and reduced magnetic helicity (bottom panel) measured in the spacecraft frame The wave activity can be seen clearly in the bottom two panels aspatches of intense amplitude and helicity between DOY 3094 and 30985 The black line across the bottom two panels is the proton gyrofrequency Doppler-shiftedinto the spacecraft frame

The Astrophysical Journal 8196 (9pp) 2016 March 1 Wicks et al

Figure 11 Example date with long-duration ion cyclotron waves (ICWs) simultaneously observed with a driftingproton beam by Wind The panels shown are the following (in order from top-to-bottom) magnetic field magnitude(magenta) and GSE components magnetic field latitude (blue) and longitude (red) Bz dynamic power spectrumand reduced magnetic helicity The black line across the bottom two panels is the proton gyrofrequencyDoppler-shifted into the spacecraft frame (Adapted from Figure 1 in Wicks et al [2016])

of all major particle populations (proton core pro-ton beam electrons alphas) contribute to the in-stability with protons dominating the anisotropyand drifts contributing more than half in the pres-ence of a proton beam (see Figure 10) Using thetheoretical long-wavelength mirror condition protonswere also found to dominate this instability but withnon-proton species contributing more than one thirdOverall this multi-species examination of these insta-bilities enabled by the high-quality instrumentationand large data set of Wind showed that the combinedthresholds work well in constraining the solar windparameters These results are important for under-standing how the instabilities operate and how theyconstrain plasma evolution both in the solar windand in other astrophysical environments where directmeasurements are not possible

Another recent study found a more direct relation-ship between the in situ particle velocity distribu-tions and electromagnetic wave activity Wicks et al[2016] examined a long-duration ion cyclotron wave(ICW) storm observed simultaneously with a sec-ondary drifting proton beam (ie drifting relative tothe core solar wind protons) Figure 11 shows datafrom the interval of the ICW storm

Using linear Vlasov theory the group found thatthe observed proton distributions were unstable to atemperature anisotropy instability (ie Tperp gt T ) ofboth the core and proton beam During some inter-vals only the core or beam satisfied Tperp gt T but dur-ing the intervals with the most intense wave activityboth satisfied this constraint The authors also foundthat the wave and beam kinetic energy densities werepositively correlated

Similar instability studies were carried out by Garyet al [2016] and Jian et al [2016] Using the well-calibrated (core and beam) proton and alpha particledata from Wind -SWE and the high-cadence magneticfield data from Wind -MFI they studied the left-handpolarized Alfven-cyclotron instability driven by anion temperature anisotropy and the right-hand po-larized magnetosonic instability driven primarily byrelative flows between different ion components Thestudy by Jian et al [2016] was carried out duringperiods of fast solar wind and that of Gary et al[2016] during slow solar wind They found some ofthe enhanced magnetic field fluctuations were consis-tent with the radiation of ICWs ndash characterized byleft-hand circular polarization parallelanti-parallel(with respect to Bo) propagation and frequency nearthe proton cyclotron frequency ndash from the Alfven-cyclotron instability In a minority of events theobserved wave modes were consistent with magne-tosonic waves ndash characterized by right-hand circularpolarization parallelanti-parallel propagation andfrequencies extending well beyond the proton cy-clotron frequency ndash radiated by the magnetosonic in-stability The non-thermal ion velocity distributionfeatures were found to be the source of free energyfor both instabilities

The solar wind electron velocity distribution func-tion exhibits a variety of features that deviate fromthermal equilibrium These deviations from equilib-rium provide a local source for electromagnetic fluc-tuation emissions including the commonly observedelectron whistler-cyclotron and firehose instabilitiesAdrian et al [2016] presents a systematic analysis ofWind -SWE-VEIS observations of solar wind electron

11 of 44

plasma and associated Wind -MFI observed magneticfluctuations

Figure 12 presents a statistical overview of theWind -SWE-VEIS observations of the solar wind elec-tron distribution occurrence frequency and normal-ized magnetic fluctuation amplitudes sorted by fast(V sw ge 500 kms) and slow (V sw lt 500 kms) so-lar wind speed The data are plotted against the-oretical thresholds for parallel propagating electroncyclotron-whistler instability (black lines for γ =10minus1 Ωce γ = 10minus3 and 10minus4 Ωce) obliquely propa-gating electron whistler-mirror mode instability for θ= 40 (dark gray dashed line for γ = 10minus3 Ωce) andthe parallel electron firehose instability (light graydashed lines for 10minus4 Ωce) that have been derived byVinas et al [2015] assuming both bi-Maxwellian (M)and Tsallis kappa-like (κ) electron distributions Thelocation of the maximum occurrence pixel of each dis-tribution has been indicated using an open-Maltesecross The bottom row of Figure 12 presents the dis-tribution of normalized magnetic fluctuation ampli-tudes (δBBo) as a function collisional age (AE) forslow (left) and fast (right) solar wind Note that thedistribution of normalized fluctuation amplitudes forslow solar wind remains relatively flat with respectcollisional age with a centroid located at sim 70times10minus3The distribution for fast solar wind is quite distinctwith its collisional age limited to values below 60 andpossessing a broadenedelongated distribution of am-plitudes centered at a collisional age of AE sim 6

For the first time Adrian et al [2016] exploit thefull solar wind electron distribution function and itsmoments without separation of the various electroncomponents (ie core halo and strahl) and find ev-idence that the temperature anisotropy threshold ofthe parallel electron cyclotron anisotropy instability(or parallel whistler anisotropy instability) boundssolar wind electrons during slow solar wind periodsFurther these authors demonstrate that during peri-ods of slow solar wind collisions while infrequent arethe dominant mechanism by which solar wind elec-trons are constrained leading to isotropization Dur-ing fast solar wind periods magnetic fluctuations andsolar wind anisotropies are enhanced above the par-allel whistler anisotropic threshold boundary and col-lisional effects are significantly reduced Preliminarycalculations presented by Adrian et al [2016] showthat the oblique electron whistler mirror anisotropicinstability bounds both the slow and fast solar windRegardless of speed the solar wind electron thermalanisotropy appears globally bounded by the parallelelectron firehose instability for anisotropies T eperpT e

lt 1 The results of Adrian et al [2016] indicate thatcollisions while infrequent play a necessary role in

regulating the solar wind electron velocity distribu-tions In striking contrast to solar wind ions solarwind electron plasma when considered globally as asingle electron velocity distribution function is onlymarginally stable with respect to parallel propagatinginstabilities

While the work presented by Adrian et al [2016]makes it tempting to establish analogies betweentheir results for electrons and those of protons re-ported by Bale et al [2009] one must remember thatthe thermal properties of electrons are very differentfrom those of ions including their characteristic timesand spatial scales for wave-particle interactions Fur-thermore the collisional processes that control theelectrons and protons occur on very different scalesas clearly demonstrated by the results of Adrian et al[2016]

The conclusions presented by Adrian et al [2016]must also be taken with some level of caution Whilethe volume of solar wind electron data consideredby Adrian et al [2016] is comparable to that pre-sented by Bale et al [2009] for solar wind protonsthe electron data considered by Adrian et al [2016]only encompass sim5 of a solar cycle in contrast tothat of Bale et al [2009] As such solar cycle phaseeffects cannot be addressed through the analysis pre-sented by Adrian et al [2016] and there is evidence inthe SWE-VEIS data from the first Wind orbital ele-ment identified that suggests ndash but not presented intheir manuscript ndash that an organization of the dataas a function of Carrington rotation exists Futurestudies are underway to incorporate additional vi-able independent SWE-VEIS electron plasma obser-vations from the remaining fifty-three Wind orbitalsegments identified by Adrian et al [2016] into theresults presented in their original work In additionthese authors have launched efforts to separate theSWE-VEIS solar wind electron plasma observationsinto their basic constituents ndash core halo and strahl ndashand in an effort to repeat their analysis for each com-ponent separately thereby systematically replicatingthe efforts of Stverak et al [2008] but in far greaterdetail

It is important to note that the three studies byChen et al [2016] Wicks et al [2016] and Adrianet al [2016] were only possible because of the mas-sive number of observations accumulated by the Windspacecraft For instance the separation of the pro-ton core and beam is a newer data product thatrequired large statistics to distinguish a secondaryproton beam from the more typical drifting alpha-particle population

While many studies in recent years rely upon Windonly as a solar wind monitor it is important to rec-

12 of 44

10ndash3 Ωe

Electron CyclotronWhistler Instability

θ = 0deg10ndash1 Ωe

10ndash4 Ωe

Electron MirrorMode Instability

Electron FirehoseInstabilityθ = 0deg 10ndash4 Ωe

855607 DATA POINTS

SLOW SOLAR WINDVSW lt 500-kmbullsndash1

496179 DATA POINTS

FAST SOLAR WINDVSW ge 500-kmbullsndash1

Figure 12 A statistical overview of the Wind SWE-VEIS observations of the solar wind electron distributionoccurrence frequency organized as a function of parallel electron beta (βe) and electron temperature anisotropy(T eperpT e) in the top row and the normalized magnetic fluctuations (δBBo) as a function collisional age (AE) inthe bottom row for slow solar wind speed (V sw lt 500 kms left column) and fast solar wind (V sw ge 500 kmsright column) Over plotted in the top row are labeled instability thresholds discussed in the text (Adapted fromFigures 3 and 9 in Adrian et al [2016])

ognize that despite its 22+ year age Wind continuesto produce new and exciting results These studiesillustrate the importance of Wind as a highquality stand-alone space plasma laboratorybecause it is the only spacecraft continuouslyin the solar wind capable of making such mea-surements

24 PSG 4 Dust ScienceIt was only recently that researchers realized that

a certain type of impulsive ldquospikeyrdquo waveform sig-nal observed the WindWAVES time domain sampler(TDS) receiver was the product of hypervelocity dustimpacts It was later determined that the signals cor-responded to micron-sized (ie dust grains approxi-mately sim1 microm in size) interplanetary dust (IPD) andinterstellar dust (ISD) [eg Malaspina et al 2014]The relevance of dust to the heliospheric communityhas increased in recent years with the recognition thatit plays an important role in numerous ways frommass momentum and energy transport to physical

damage to spacecraft (eg cutting of wire antenna)There are two potential mechanisms proposed to

explain the impulsive electric field signatures ob-served by waveform capture instruments (1) thespacecraft body changes electric potential after theimpact but the antenna do not and (2) the chargecloud produced by the impact interacts with the an-tenna directly It was only recently determined thatboth mechanisms are at play on Wind [Kellogg et al2016] This was determined by comparing the dustflux rate early in the mission to that later in the mis-sion The reason is that one side of thesim100 m tip-to-tip wire antenna (x-antenna) was cut (it is assumedby dust) twice once on August 3 2000 and the sec-ond time on September 24 2002 Thus prior to thefirst cut the x-antenna responded as an electric dipoleand was insensitive to changes in the spacecraft po-tential During this period the number of impactswas lower by factors sim15ndash30 compared to periodsafter the cut Therefore it appears likely that the

13 of 44

2017 Wind Senior Review New Prioritized Science Goals

second mechanism may contribute more to the totalnumber of dust impacts than the first

Daily Total TDS and Dust Impacts for Duration of Wind Mission

Total of TDS 1429672

1994 1996 1998 2000 2002 2004 2006 2008 2010 2012 2014 2016 2018Year

102030405060

Figure 13 Plot of the entire Wind mission showing thedaily totals In each panel the dark blue and red linesrepresent the actual and 10-day smoothed countsrespectively The panels shown are the following (inorder from top-to-bottom) total number of TDS eventsper day number of dust impacts observed on thex-antenna and number of dust impacts observed on they-antenna The two vertical green lines define thecurrent duration of the Wind mission The two verticalcyan lines define the times when the x-antenna was cut(Adapted from Figures 5 and 6 in Malaspina and WilsonIII [2016])

Figure 13 shows the counting statistics for TDSevents and dust impacts observed by the Wind TDSreceiver The obvious annual variation in dust im-pacts seen in the bottom two panels is primarily dueto ISD The reason is that for half of the year Windis moving approximately anti-parallel to the flow ofISD through the solar system The difference in flowspeed of the ISD in Wind rsquos reference frame variesfrom sim4ndash56 kms thus leading to an annual variationin the counting rates (ie higher impact speeds pro-duces larger electric field amplitudes and thus moredust observations) This annual variation has beenreported in multiple studies [eg Kellogg et al 2016Malaspina and Wilson III 2016 Malaspina et al2014 Wood et al 2015]

Wind is a south-ecliptic spin-stabilized spacecraftThis allowed Malaspina et al [2014] to estimate a thedirection from which the incident dust must have ar-rived Both Malaspina et al [2014] and Wood et al[2015] found that their estimates of the ISD impactdirection were consistent with the expected interstel-lar flow direction Thus the annual variation in dustimpacts is entirely due to ISD as IPD has no pre-ferred direction in the solar rest frame With thelarge number of impacts recorded by Wind due to itslongevity and relatively large impact target area (iethe spacecraft bus) it was also determined that Wind

does not respond to nanodust (ie grains with 01microm in size) [eg Kellogg et al 2016 Malaspina andWilson III 2016 Malaspina et al 2014]

These results illustrate Wind rsquos unique capabilitiesand the importance of its longevity For instanceWind independently verified the direction ofISD flow showing it agrees with predictionsand results from Ulysses a critical piece of in-formation for current and future heliosphericand astrophysical missions These results haveimproved our understanding of the interactionbetween the heliosphere and the local inter-stellar medium

25 Noteworthy StudiesUnfortunately there is not sufficient room to ex-

plain in detail all the new and exciting work per-formed since the last Senior Review However wethought it necessary to mention several works thatwere not explicitly discussed in our PSG progress re-ports from the previous sections Some of the workbelow derived from Wind rsquos unique complement ofinstruments (eg the KONUS gamma-ray detector)while others were outside the scope of our prior PSGsRegardless we thought it necessary to at least brieflymention these studies in the short list shown below

1 Highlight on ultra-long-duration gamma raybursts [Greiner et al 2015]

2 Discovery of electron acceleration to relativistic en-ergies in ion foreshock [Wilson III et al 2016]

3 Highlight on solar wind reconnection [Xu et al2015]

4 Shock acceleration of electrons during large SEPevents [Tan and Reames 2016]

5 Shock acceleration of heavy ions [Gruesbeck et al2015 Nitta et al 2015 Wang et al 2016]

6 Relationship between solar radio bursts andICMEs [Salas-Matamoros and Klein 2015Suresh and Shanmugaraju 2015 Vasanth et al2015]

7 SEP solar flare and ICME dependence upon SC[Dierckxsens et al 2015]

8 Electron superhalo observations during quiet solarwind periods [Wang et al 2015]

3 New Prioritized Science Goals

New Prioritized Science Goals1 Wave- andor Turbulence-Particle Studies2 Unusual Solar Cycle3 Particle Acceleration4 Long-Term Dust Science

Again we emphasize that the Wind mission is op-erating on a minimal budget that does not allow for

14 of 44

the dedicated support of any in-depth focused scien-tific research (eg see Section 6) In the followingsections we outline a number of prioritized and fo-cused science research topics that the Wind instru-ment teams are planning to undertake during thenext five years as per the proposal call

31 Field-Particle StudiesWind still retains some of the highest resolution

measurements of near-Earth spacecraft and is theonly L1 spacecraft capable of measuring both DC-and AC-coupled electric and magnetic fields Theseunique measurements make Wind a unique observa-tory for examining the kinetic physics involved in theinteraction of particles with fluctuating electromag-netic fields whether coherent wave modes or turbu-lence In this section we introduce some novel ideasfor future Wind investigations combining measure-ments of both electromagnetic fields and particle ve-locity distributions

311 Turbulence Studies

Wind shares a instrument suite similar to that ofSolar Probe Plus (SPP) which will allow for com-parative analysis of measurements from each set ofinstruments For instance during periods of nearlyradial conjunction tests of the evolution of turbu-lence and particle velocity distributions will be pos-sible Of particular interest will be cross-comparisonstudies between Wind and other missions like ACEDSCOVR SPP and Solar Orbiter (SolO) to exam-ine the large-scale dynamics of solar wind turbu-lence Constraints provided by long intervals of thesesystem-scale multipoint observations will enable com-parisons with global solar wind simulations drivenby magnetograms and corona observations [Lionelloet al 2014 Usmanov et al 2014] Long baselinecorrelations of electron observations from inner helio-spheric observations (SPP) and Wind electrons willenable studies of magnetic field line topology andwandering These studies will be able to quantifythe effects of turbulence over 1 AU scales a crucialelement for estimating error in Space Weather pre-diction

Wind also plays an important role in a recently im-plemented [Matthaeus et al 2016] method for under-standing the intrinsic time dependence of solar windmagnetic field turbulence This method also enablesdirect examination of the accuracy of the Taylor hy-pothesis (ie the frozen-in flow approximation) thatallows researchers to convert temporal observationsinto spatial correlation After accumulating numer-ous datasets this method provides the full space-timecorrelation (in the plasma frame) Although not pre-cise for any individual data interval for a suitable

defined ensemble such as slow wind or fast windthe method permits study of the breakdown of theTaylor hypothesis at various scales This approachemploys many pairs of multi-spacecraft observationalintervals and becomes more useful and accurate asthe ensemble becomes better populated This studyprovides a useful database that can help interpret thesingle spacecraft datasets obtains by Solar Probe Plusand Solar Orbiter As this fundamental dataset isaccumulated and improved it can provide predictionsfor effects of time decorrelations that will be observedduring near-radial alignments of the constellation ofheliospheric spacecraft including Wind

The partition of energy between electrons pro-tons and minor ion species is a major issue in un-derstanding the acceleration and extended heating ofthe solar wind and the heating of the corona Wind rsquosunique set of thermal plasma measurements providean invaluable testbed for the very active theoreti-cal and simulation work on this fundamental sub-ject For example the ratio T eT p provides con-straints for both turbulence and kinetic plasma the-ory Further Wind rsquos newly calibrated electron datacombined with T p and Bo can be used to furtherpin down heating rates due to turbulence and relatethem to theory [eg Matthaeus et al 2016] Thesame approach using large datasets may be used totest theoretical developments that aim to predict howthe heating rates and partition of energy betweenelectron and protons can be related to inertial anddissipation range properties A common thread inthese developments is that stronger turbulence shouldproduce more significant coherent structures at ionscales This can lead to greater distortions in theparticle distributions fueling additional kinetic pro-cesses eventually leading to heating andor acceler-ation Our current understanding suggests that co-herent structures tend to increase the intermittencyand local heating in the plasma Local heating atproton scales appears to be correlated with steepersub-proton scale spectra as well as large magneticfluctuation amplitudes at the proton gyroscale Tur-bulence remains an active and important topicin understanding the structure and dynamicsof the heliosphere and Wind data has beencentral in many of the basic studies that havebeen done and that are planned to be doneparticularly in the new SPP and SolO era

312 WaveInstability Studies

Given the recent increased interest in kineticscale phenomena Wind rsquos importance to the com-munity has only increased Wind rsquos 22+ year agewill allow researchers to perform both case stud-ies [eg Wicks et al 2016] and long-term statis-

15 of 44

tical studies [eg Adrian et al 2016 Chen et al2016] of waveinstability interactions with particlesThe results from past studies have already helpedto improve the science definitions for future mis-sions like SPP and SolO Further many of thewaveinstability-particle studies using Wind are usedas critical tests and constraining criteria for the devel-opment of new missions like the Interstellar MAppingProbe (IMAP) and Turbulence Heating ObserveR(THOR)

With the release of the entire electron distribu-tion function moments (ie account for spacecraftpotential) and the future release of the velocity mo-ments of the electron components (ie core haloand strahl) tests of waveinstability-particle interac-tions will be more readily available We expect thesenew higher level data products to improve the sci-ence return of Wind and future missions Furtherthe necessary enhancements in time resolution formissions like SPP and SolO arose by necessity be-cause the time scales for the same phenomena at 1AU decrease with decreasing distance from the sunThe time resolution of many of Wind rsquos instrumentsare comparable to SPP and SolO when normalized tophysical parameters (eg local cyclotron frequency)Thus Wind will continue to play a critical rolein the study of kinetic physics resulting fromwaveinstability interactions with particles

313 New Analysis Techniques

As the community becomes increasingly aware ofthe relevance of kinetic-scale processes to the evolu-tion of the solar wind and other macroscopic phe-nomena (eg collisionless shocks) the need for thecontinued operation of Wind becomes more obviousThe instrument teams continue to improve the cali-bration and accuracy of the measurements each yearbecause the increasing number of data points reducesthe statistical uncertainties in many parameter cal-culations Below we highlight a specific new analy-sis technique that will be employed in wave- andorturbulence-particle studies over the coming years

Typically the analysis of particle velocity distri-bution functions requires a strong technical under-standing of the instrument and calibration schemesThus these steps have traditionally been carried outby the instrument teams using semi-automated anal-ysis software The automated routines are optimizedfor typical solar wind conditions so they can fail tocapture the complex (and scientifically interesting)microphysics of transients in the solar wind (egCMEs) which are often better analyzed manually

The recently released publicly available(httpsgithubcomJanusWindFC) Janus soft-ware (created by Bennett Maruca funded under

NASA Awards NNX15AF52G and NNX17AC72G)is now providing the scientific community with a newparadigm for analyzing thermal ion measurementsfrom Wind and other spacecraft Janus providesusers with an easy-to-use graphical user interface(GUI) for carrying out highly customized analyses ofion velocity distributions without need for detailedbackground information or prior knowledge of theinstrument idiosyncrasies This will allow users fromthe entire community to examine the thermal ionvelocity distributions in detail for the first time

0 2000 4000 6000 8000 10000

minus10

minus5

~ B[nT]

10minus3

10minus2

10minus1

minus3]

minus30

minus20

minus10

v jminusv

p[kms]

330 400 430 500 530 600

Time on 2002-07-05

Tj[kK]

Figure 14 From Maruca et al [2016] selectparameters from the Janus analysis of an exemplarperiod of FC measurements of the solar wind From topto bottom these plots show the magnetic field (fromWindMFI) ion density ion differential flow (relativeto protons) and ion temperature For protons andα-particles the plotted values are of ldquototalrdquo parameterswhich incorporate both the beam and core populations

Version 1 of Janus released late last year [Marucaet al 2016] focuses specifically on measurementsfrom the WindSWE Faraday Cups (FC) Thoughthe moments and reduced distribution functionsfrom the SWE-FCs has been publicly available onCDAWeb Janus allows the user to perform their ownanalysis on the thermal ion velocity distributions

16 of 44

Figure 14 presents an example output from Janusof FC measurements from a particularly dense (n

pasymp

30 cmminus3) period of slow (Vpasymp 350 kms) solar wind

The high density allowed the FCs to resolve a thirdspecies O6+ in addition to the usual protons andalpha-particles Both the protons and alpha-particlesexhibited distinct core and halo components givinga total of three species and five populations analyzedThe density trends for these three species were verysimilar suggesting a steady relative abundance Fur-ther the drift between the protons and both thealpha-particles and O6+ were very similar thoughthe latter tended to be slightly faster The ion tem-peratures were consistently ordered by particle mass(with O6+ usually hottest) but the relationship wasless than mass proportional (possibly due to colli-sional thermalization) [Kasper et al 2008 Marucaet al 2013]

Two extensions of Janus are now under develop-ment First the team is adapting Janus to ana-lyze the 3DP thermal ion measurements from the twoelectrostatic analyzers (ESAs) called PESA Low andHigh The two PESA instruments can resolve a full3D velocity distribution from a few 10s of eV to sim30keV which will allow users to explore the ion velocitydistribution functions for evidence of non-Maxwellianfeatures (eg kappa and skew-normal distributions)

Second Janus will be expanded so that it canjointly process measurements from the FCs andPESA Low This will be the first time that data fromFCs and ESAs have been combined It will draw uponthe strengths of each detector to produce higher qual-ity solar wind ion parameters Furthermore this willserve as an important case study for SPP [Fox et al2016] which will also have both a FC and an ESA formeasuring thermal ions However unlike their coun-terparts on Wind the SPP instrument fields-of-viewwill only slightly overlap For instance SSP is fre-quently expected to encounter periods during whichthe combined FC and ESA measurements will providenearly complete coverage of the thermal ions but willnot individually [eg see Figure 9 in Kasper et al2016] Therefore the adaptation of the Janussoftware to perform such a joint analysis is es-pecially important and will benefit both theWind and SPP missions

32 Unusual Solar CycleAs of November 1 2016 Wind marked 22 years of

continuous operation only surpassed in age (for cur-rently operational spacecraft) by SOHO Geotail andthe two Voyagers Long-term solar cycle investiga-tions whether they are about large-scale structuresor solar wind conditions critically depend on contin-uous high quality observations These studies can be

severely hindered when multiple spacecraft are useddue to the complexities and time consuming effortsof instrument inter-calibration Therefore the con-tinuation of Wind becomes even more beneficial tothe community

Year1994 1996 1998 2000 2002 2004 2006 2008 2010 2012 2014 2016

Daily Avg Sunspot Numbers for Duration of Wind Mission

Figure 15 Daily (blue line) and 27 day smoothed (redline) average sunspot numbers (SSNs) for the duration ofthe Wind mission (defined by vertical green lines) Thedata are taken from httpwwwsidcbesilsoinfosndtot

As was previously illustrated Wind rsquos con-tinuous long-term observations have re-sulted in several lists of SC-dependent phe-nomena like ICMEs [eg Nieves-Chinchillaet al 2017] and interplanetary shocks (eghttpwwwcfaharvardedushockswi data) Thenext SCrsquos effect on these phenomena is obviouslynot known but continuation of Wind through FY22should provide statistics into SC25 The additionalinformation will help the community improve pre-dictive capabilities for space weather and long-termphenomena

As we enter an ldquounusualrdquo solar minimum follow-ing an ldquounusualrdquo solar maximum it is important tomaintain continuous coverage of the solar wind Theweaker than normal solar maximum of SC24 is evi-denced in Figure 15 It is also important to remem-ber that this solar minimummaximum will share thesame magnetic polarity as SC22 allowing for directcomparison with the early Wind measurements ofcosmic rays and elemental abundances [eg Reames1999] The magnetic polarity was also found to affectthe 27 day variations associated with solar rotation[eg Reames and Ng 2001] an effect which must beconfirmed with new observations in the impendingsolar minimum

Regardless of the predictions the operation ofWind through FY22 would provide the communitywith a continuous array of datasets that span fromthe end of SC22 to the beginning of SC25 all near-

17 of 44

Earth measurements Given that the observed andpredicted trends in solar behavior suggest we areentering a long-term solar minimum [eg Zachilasand Gkana 2015] the importance of maintaining asingle uniform dataset is further magnified Thusthe rationale for continuing the Wind missionthrough FY22 becomes obvious

33 Particle AccelerationUpstream of a magnetized collisionless shock there

can be a region in communication with the shock ndashthe foreshock ndash unlike collisionally mediated shockslike in Earthrsquos neutral atmosphere Foreshocks occurupstream of quasi-parallel magnetized shocks wherethe shock normal angle (θBn) between the upstreamquasi-static magnetic field (Bo) and the shock normalvector satisfies θBn lt 45 Foreshocks are primarilypopulated by suprathermal ions reflectedenergizedby the shock and streaming against the incident bulkflow The relative drift between the incident and re-flected ions can drive numerous instabilities [eg Wil-son III 2016] some of which are wave-like and oth-ers are structure-like For brevity let us refer to thestructure-like transient phenomena as foreshock dis-turbances ndash large-scale (sim1000 km to gt30000 km)solitary (sim5ndash10 per day) transient (lasting sim10s ofseconds to several minutes) structures [eg Omidiand Sibeck 2007 Turner et al 2013 Wilson IIIet al 2016] that are generated by the free energy inthe streaming between reflected suprathermal (gt100eV to 100s of keV) and incident solar wind ions [egBurgess et al 2012 Wilson III 2016]

The recent discovery that foreshock disturbancescan locally generate relativistic electrons up to sim300keV [eg Wilson III et al 2016] has raised severalquestions about our understanding of shock accelera-tion Some of these structures had been found to lo-cally generate field-aligned ion beams [eg Wilson IIIet al 2013] and even their own miniature foreshocks[eg Liu et al 2016] Prior to these studies it wasnot thought possible for these structures to efficientlyaccelerate electrons let alone generate energies an or-der of magnitude higher than thought possible at thebow shock Subsequent investigation of many moreforeshock bubbles has found electrons with energiesin excess of sim700 keV [Personal communication withTerry Z Liu Dec 13 2016 ]

The suprathermal ion pool between sim2ndash10 timesthe solar wind speed provides most of the seedpopulation for corotating interaction region (CIR)and CME-associated shocks in the inner helio-sphere Wind rsquos SMSSTICS EPACTSTEP andEPACTLEMT provide unique measurements ofthe composition and energy spectra of suprather-mal ions through energies between sim3 keVe - 20

MeVnucleon Thus Wind provides near-completespectral and compositional coverage of the suprather-mal seed populations as well as the accelerated pop-ulations during large gradual SEPs 3He-rich impul-sive SEPs and recurrent particle events associatedwith CIRs Using STEP data Filwett et al [2017]recently showed that the sim20-320 keVnucleon heavyion population in 41 CIRs observed from 1995ndash2008most likely originates from the re-acceleration of asim20ndash80 keVnucleon suprathermal population thatwas measured upstream a few days earlier Furtherthey found that this suprathermal population is ac-celerated within sim1 AU of Earth-orbit These resultsare at odds with the traditional model in which CIRparticles observed at 1 AU are accelerated at shocksbetween sim3ndash5 AU and then transported to Earth-orbit but are instead consistent with the more recentWind observations [eg Ebert et al 2012ab]

The solar minimum of SC25 offers an unprece-dented opportunity to combine Wind ACE andSTEREO observations with those from SPP and SolOto track the evolution of compression regions frominside sim02 AU and determine where they start ac-celerating particles In addition the Wind team willcombine observations of Type II and Type III ra-dio bursts with in-situ suprathermal and SEP datawith remote sensing data from STEREO and SDOto identify and study the properties of a variety ofsolar source regions of SEP events (eg flares jetsfilaments coronal shocks etc) During the latter por-tion of the senior review period we will use SolO andSPP to track the evolution of transients CMEs andtheir shocks and make significant progress on sepa-rating the effects of acceleration and transport thatroutinely blur the interpretation of SEP events ob-served near Earth-orbit

The unique capabilities of the 3DP SST instrumentto measure the full angular dependence of protons inthe energy range from sim100 keV up to a few MeVallows researchers to test the predictions of classicaldiffusive shock acceleration (DSA) for near-isotropicintensities against advanced models which take intoaccount the pitch-angle and gyrophase dependence aswell as focused transport and adiabatic decelerationthe solar windmagnetic field structures in the in-ner heliosphere [eg Gedalin et al 2016 Kartavykhet al 2016] The above effects can be expected tolead to measurable differences in the spectrum of theaccelerated particles as a function of the the shockangle and the compression ratio and could providefurther insight about the energization of particles atastrophysical shocks

These studies have altered our understand-ing of shock acceleration and have raised ques-

18 of 44

2017 Wind Senior Review Wind in the Heliophysics System Observatory

tions about local vs remote pre-energization(ie the so called ldquoinjection problemrdquo) Thuswe will exploit the newly processed Winddatasets from SMS EPACT and 3DP to lookfor evidence of local vs remote shock accel-eration and continue to aid with and advanceforeshock and bow shock studies

34 Long-Term Dust ScienceDavid M Malaspina (PI) and Lynn B Wilson III

(Co-I) created a dust impact database [Malaspinaand Wilson III 2016] for the entire Wind mis-sion (currently from Jan 1 1995 to Dec 312015) The database can be found at CDAWeb(httpscdawebgsfcnasagov) The Wind databaseis the only sim21 year long record of micron (ie dustgrains approximately sim1 microm in size) interplanetarydust (IPD) and interstellar dust (ISD) at 1 AU withcurrently gt107000 impacts The authors intend toupdate the database from its current state (1) in early2017 to extend it through 2016 (2) when the finalWindTDS data is sent to SPDFCDAWeb and (3)once every two years for the continuing duration ofthe mission

The publicly available database now allows re-searchers to perform long-term investigations of thephenomena (eg ICMEs) that may influence sim1 micromdust grains The database also overlaps by 12 yearswith the Ulysses dust database allowing for cross-comparison The primary advantage of the Winddatabase is that the entire spacecraft body acts as thecollecting area (ie amp43 m2 excluding topbottomdecks) in contrast to missions with dedicated dustdetectors where the effective collecting area is sim01m2 (eg Ulyssesrsquo dust instrument [eg Gruen et al1992]) Consequently Wind has recorded gt107000impacts This is over an order of magnitude moreimpacts than Ulysses (sim6700) over its 16 year mis-sion life [eg Wood et al 2015] and Cassinirsquos sim36ISD impacts over sim10 years of data [eg Altobelliet al 2016] While the Wind database does notdefine the impactorrsquos speed mass or compositionthe large number of impacts is unique and absolutelycritical for statistical studies and long-term investi-gations

Finally the database is not only useful for the he-liophysics and planetary communities it is importantfor mission planning (eg SPP and SolO) and the as-trophysics community The importance and uniquevalue of this dataset will only increase as we enteran historically unusual period of solar activity Fur-ther the planned launch of SPP and SolO is in 2018which is during the second half of this proposal pe-riod Therefore Wind can serve as a ldquostan-dard candlerdquo for dust observations to which

both SPP and SolO can compare

4 Wind in the HSOAs part of the Heliophysics System Observatory

(HSO) Wind has been contributing to numerous sci-ence investigations that rely on multi-spacecraft ob-servations Many of these have been described inthe preceding sections In addition Wind observa-tions are also critical to many other spacecraft en-abling and enhancing their mission success This isevidenced by the over 600 refereed publicationsand the gt1825000 data access requests onCDAWeb since the last Senior Review Thissection outlines some of these functions Wind serves

41 Inner Heliospheric MissionsACE

Wind and ACE have been working under mutualcalibration support for several years in order to in-crease the scientific value of each mission Wind rsquoscapacity to measure the total electron density us-ing the WAVES radio receivers to observe the upperhybrid line (or plasma line) is unique among everyL1 spacecraft and most near-Earth spacecraft (VanAllen Probes and MMS have this capacity as well)This unambiguous measurement of the total electrondensity coupled with two independent thermal ionplasma measurements (3DP and SWE) give Windthree separate measurements for cross-calibration re-sulting in highly accurate thermal plasma observa-tions Further the SWE instrument can operateeven during intense high energy particle events as-sociated with solar flares and CMEs The robustnessof Wind rsquos instrumentation and measurements makesit a invaluable asset for near-Earth solar wind mon-itoring and other spacecraft For instance the ACESWEPAM team uses Wind rsquos thermal plasma obser-vations to help improve their calibrations We ex-pect to continue this cooperation for the foreseeablefuture

The spin axes of Wind and ACE are orthogonal toeach other which provides a very useful opportunityfor magnetic field cross-calibration The spin planecomponents of fluxgate magnetometers are the mostaccurate so the two spacecraft use the orthogonalityof their spin planes to their advantage during periodswhen the two spacecraft are in near proximity to eachother

ACE has a much more robust and wider coverage ofenergies for high energy particle observations How-ever the EPACT-LEMT telescope on Wind can ob-serve particles in the sim1ndash10 MeVnuc range whichfalls between the ULEIS and SIS detectors on ACEFurther the ecliptic south spin axis of Wind allowsthe LEMT telescope to determine anisotropies in the

19 of 44

high energy particles (eg it can detect particlesstreaming sunward from the outer heliosphere) Fi-nally the larger geometric factor of EPACT allows itto observe less intense solar energetic particle events

In summary Wind provides significant andunique calibration information for ACE com-plements its measurements and facilitates col-laborative multi-spacecraft studiesDSCOVR

The Deep Space Climate Observatory (DSCOVR)was launched on Feb 11 2015 DSCOVR is taskedto provide solar wind proton and magnetic field mea-surements from L1 (the same region where WindACE and SOHO operate) for NOAA space weatherprediction purposes

Wind has been an essential calibrator for DSCOVRand is the primary reference for DSCOVR plasmadata trending and anomaly tracking The DSCOVRPlasMag Faraday Cup (FC) is a plasma diagnosticinstrument of central importance to real time spaceweather monitoring modeling and forecasting ef-forts The sensor is physically identical to the WindSWE FCs in most respects and operates in a similarmode but it is perpetually sun-pointed In 2015ndash2016 during the extended commissioning period forthe instrument grounding and charging anomaliesthreatened to render the DSCOVR instrument un-usable Wind SWE measurements of solar wind pro-tons were used as a standard for a full recalibrationof the DSCOVR FC response a characterization ofthe anomalous backgrounds and a revision of the op-erating mode such that it could meet requirements

As DSCOVR has been accepted and transitionedto space weather operations the Wind spacecraftcontinues to provide the standard against which theDSCOVR measurement consistency and quality areevaluated Properly calibrated the relatively highcadence measurements from both the FC and themagnetometer on DSCOVR provide an interestingcompliment to the Wind measurements The Wind -DSCOVR comparison also constitutes a new baselinefor multi-point studies of solar wind structures nearL1 completing a tetrahedral solar wind constellationwith SOHO and ACE that is suitable for planar tim-ing analysis on scales comparable to the solar windcorrelation scale [eg Weygand et al 2009] Publicrelease of science-grade data from DSCOVR beganin late 2016 enabling joint Wind -DSCOVR investi-gations to beginSTEREO

With the recent return of communications withSTEREO-Ahead after passing behind the sun and theinterrupted communications with STEREO-BehindWind continues to be one of only three inner helio-

spheric missions with radio observations of the sun(ie Wind MAVEN and STEREO-Ahead) Withthe ending of MESSENGER in April 2015 and VEXin January 2015 Wind rsquos importance in global helio-spheric observations has greatly increased Until therecovery of STEREO-Behind Wind MAVEN andSTEREO-Ahead will be the only inner heliosphericradio observatories (though radio bursts need to bevery strong to be observed by MAVEN) With thecurrent non-viability of STEREO-Behind Wind isacting as the stereo-partner of STEREO-Ahead forcurrent studies particularly because of the similaritiesin their instrumentation Thus Wind continuesto be and will remain a critical component inthe HSOMAVEN

The Mars Atmosphere and Volatile EvolutioN Mis-sion (MAVEN) designed to study the Martian atmo-sphere arrived at Mars (sim15 AU) on September 222014 Mars remained on the far side of the sun rel-ative to Earth until early 2016 It is currently sim90

from Earth Thus Wind MAVEN and STEREO-Ahead form a unique constellation currently spanningsim180 allowing for inndashsitu plasma and remote radiomeasurements of large transients in the inner helio-sphere for both observational and simulation studiesof space weather

42 Solar Probe Plus and Solar OrbiterSolar Probe Plus (SPP) and Solar Orbiter (SolO)

are not planned to launch until 2018 thus their pri-mary mission starts during the second half of thisproposal period Even so Wind continues to pro-duce significant and relevant studies helping to im-prove the future science output and predictionstestsfor these two flagship missions Only the high reso-lution of Wind measurements can provide an appro-priate 1 AU baseline for SPP and SolO observationsDSCOVR is expected to exhaust its propellant aftersim5 years and has limited measurements (ie onlymagnetic fields and thermal ions) For comparisonWind has gt50 years of fuel The short sim88 day or-bit of SPP and the sim03ndash076 AU orbit of SolO willprovide frequent radial and magnetic alignment withWind allowing for multi-spacecraft studies This willsignificantly enhance the science return of both SPPand SolO

The primary scientific goal of SPP is to determinethe processes responsible for heating and accelera-tion of the solar corona and solar wind These pro-cesses (eg instabilities wave-particle interactions)tend to take place on very small time scales near theSun barely resolvable even by the extremely high ca-dence SPP instruments However near 1 AU thesame processes operate slower making their observa-

20 of 44

tion by Wind possible Towards the next solar max-imum particle and plasma observations from WindSPP and SolO during periods when all three space-craft are radially or magnetically aligned will allowresearchers to study the radial variation of particleacceleration at interplanetary shocks of the trans-port coefficients governing the propagation of solarenergetic particles and the evolution of the magneticturbulence in the solar wind from 10 R to 1 AU

Thus Wind will continue to help identifylocal vs remote heating and accelerationprocesses complementing the observations ofWind and STEREO-AB during the past so-lar cycle for longitudinal variations of plasmaand energetic particle observations and willcontribute essential to both SPP and SolO

43 IBEX and VoyagerWind observations have usually supplied the 1

AU baseline for deep space observations (eg thetwo Voyager spacecraft) since the IMP 8 magne-tometer stopped returning data in 2000 The ro-bust and continuous solar wind measurementsfrom Wind are essential for studies rangingfrom the predicted position of the terminationshock and heliopause also observed remotely byIBEX to the evolution of solar wind transientsfrom the inner-to-outer heliosphere

44 Magnetospheric MissionsNearly all magnetospheric investigations utilize in

some way data from an upstream solar wind mon-itor This is partly evidenced by the gt1825000access requests registered by CDAWeb (gt350000for HTTP and gt1450000 for FTP access) for Windand OMNI data (which largely relies upon Wind andACE measurements) between Jan 1 2015 and Jan1 2017 Missions that have continue to and willrely upon Wind for solar wind data include ClusterTHEMIS ARTEMIS Van Allen Probes and MMSTherefore Wind will remain a crucial element inmagnetospheric studies through 2017THEMIS

The two THEMIS spacecraft in permanent lunarorbits called ARTEMIS spend a large fraction oftheir time in the ambient solar wind This allows forhigh quality multi-spacecraft solar wind studies egdetermining the large-scale structure of interplane-tary shocks [Kanekal et al 2016]

All five THEMIS spacecraft are equipped with highcadence (sim3s in burst mode) plasma distributionfunction observations allowing for very precise multi-spacecraft studies Wind provides a critical moni-tor of the interplanetary environment for interpreta-tion of THEMIS measurements For instance the

recent discovery of relativistic electrons generated lo-cally within the ion foreshock [Wilson III et al 2016]relied heavily on Wind radio and energetic particleobservations to rule out a solar source

It is worth noting that THEMIS used Wind tocalibrate its thermal plasma instruments [McFaddenet al 2008ab] since its electric field receivers couldnot consistently observe the upper hybrid lineVan Allen Probes and MMS

The two Van Allen Probes and the four MMSspacecraft launched on August 30 2012 and March13 2015 respectively Both of these missions relyheavily upon solar wind monitors for various rea-sons (eg determining the distance to the magne-topause from MMS) as evidenced by the increas-ing Wind publications per year (ie gt330 in 2016alone) Further the Van Allen Probes Science Work-ing Group identified a need for solar wind obser-vations to achieve its scientific objectives ThusWind will continue to provide high quality so-lar wind observations required for the numer-ous magnetospheric studies by the Van AllenProbes and for the MMS missions

45 Solar and AstrophysicsSolar Flares

During itrsquos more than 22 year-long historythe KONUS instrument onboard Wind has ac-cumulated an unique volume of solar flare ob-servations in the hard X-ray and gamma-rayrange Data on solar flares registered byKONUS in the triggered mode are published online(httpwwwiofferuLEAkwsun) This database(named KW-Sun) provides light curves with hightemporal resolution (up to 16 ms) and energy spec-tra over a wide energy range (now sim20 keV tosim15 MeV) The high time resolution of KONUS al-lows for the study of fine temporal structure in so-lar flares and the KONUS energy band covers theregion of non-thermal emission from electrons andions in solar flares that allows probing their ac-celeration mechanisms New solar observations willbe added to the database as soon as they arriveThe list of KONUS triggered-mode solar flares from1994 till present time along with their GOES clas-sification is automatically updated and available athttpwwwiofferuLEASolarRHESSI

RHESSI provides imaging and spectroscopy of thehard X-rayγ-ray continuum and γ-ray lines emittedby energetic electrons and ions respectively Windcomplements RHESSIrsquos observations using remoteobservations of radio (WAVES) and γ-rays (KONUS)in addition to inndashsitu measurements of energetic par-ticles (3DP SMS and EPACT) Thus Wind can pro-

21 of 44

vide a secondary remote and primary inndashsitu observa-tory of solar flares and the associated energetic parti-cles respectively Wind will continue to support thisand similar RHESSI research projectsSwift and Fermi

Cosmic gamma ray bursts (GRBs) are the bright-est electromagnetic events known to occur in the uni-verse occurring transiently from the collapse of mas-sive stars or coalescence of compact objects (eg twoneutron stars or a neutron star-black hole merger) inthe early universe GRBs consist of an initial flash ofgamma-rays lasting from milliseconds to minutes fol-lowed by a longer duration ldquoafterglowrdquo at radio andoptical wavelengths About 120 per year are detectedby KONUS (almost 3000 to date)

Soft gamma repeaters (SGRs) are strongly magne-tized Galactic neutron stars (surface fields up to 1014

G) that emit large bursts of X-rays and gamma-raysat irregular intervals There are presently only abouttwo dozen known SGR sources When they becomeactive they emit bursts from a few times up to hun-dreds of times over spans from days to months

SGR Giant Flares (GFs) are of greater apparentintensity than GRBs and are very rare averagingonce per decade Only a handful have been detectedto date and their intensities are sufficient to cre-ate easily detectable ionospheric disturbances indeedKONUS has detected both GFs from SGR 1900+14and SGR 1806-20 KONUS has also detected a GFfrom the Andromeda Galaxy

KONUS was designed to study GRBs SGRsand GFs with omnidirectional unoccultedsensitivity It also has broadband sensitivitycoupled with excellent time- and energy resolu-tion For over two decades it has been a keycomponent of the Interplanetary Network (IPNhttpsslberkeleyeduipn3indexhtml) main-tained by Dr Kevin Hurley which determines thesource directions of transients by triangulation Theprimary spacecraft involved in the IPN are WindMars Odyssey INTEGRAL RHESSI Swift andFermi KONUS extends the energy range of Swiftfrom 150 keV to 10 MeV a crucial data set for aglobal understanding of gamma-ray transients anddetects events which are Earth-occulted to FermiIn addition it is generally the most sensitive of theIPN detectors to SGRs (sim350 detections to date)due to its lack of collimation and Earth occultationand broad energy coverage

KONUS remains a very active partner in theGamma-ray Burst Coordinates Network or GCN(httpsgcngsfcnasagov) maintained by Dr ScottBarthelmy (NASA-GSFC) The GCN circulates in-formation on bursts rapidly to thousands of as-

tronomers worldwide who conduct multi-wavelengthand now also neutrino and gravitational wave follow-up observations Indeed with the first detection ofgravitational radiation by LIGO in 2016 KONUSand the IPN have taken on a new role ndash the search forgamma-ray transients associated with gravitationalwave sources such as the inspiral of two neutron starsin a binary system As LIGOrsquos sensitivity increasesover the coming years the first such detection be-comes increasingly likely ushering in a new era ofastrophysical observations As high energy neutrinodetections are now becoming more common a similarsymbiosis exists for them Thus the instrument re-mains a unique active and irreplaceable contributorto the astrophysical community Due to the rar-ity of these astrophysical events an additionaltwo years of Wind KONUS observations willsignificantly enhance the events collected bySwift Fermi the IPN and the GCN

46 Wind CCMC and CDAW

The Coordinated Community Modeling Center(CCMC) is tasked to validate heliophysics modelsIn particular terrestrial magnetospheric models aredriven by solar wind input The accuracy of this in-put especially during extreme solar wind conditionsis critical for the proper evaluation of the modelsHistorically Wind measurements have been used asthe standard It is expected that as the complexityincreases in future models their sensitivity to the un-certainties of driving conditions will increase ThusWind measurements will continue to be an es-sential input for the CCMC model validationprogramWind and CDAW Data Center

The CDAW Data Center is a repository of CMEsradio bursts and associated phenomena related tospace weather (httpscdawgsfcnasagov) TheData Center provides an online catalog of all CMEsmanually identified from SOHOLASCO imagessince 1996 and all type II radio bursts observed byWindWAVES (link found on Wind webpage and inAppendix A) with links to the corresponding CMEsthat produced the type II bursts There are alsodaily movies that combine SOHOLASCO imageswith WindWAVES dynamic spectra to identify theconnection between CMEs and Type II III and IVradio bursts (eg Dynamic Movie Creator) Thesmall subset of Type II producing CMEs have beenfound to play a critical role in space weather [egVasanth et al 2015] and solar energetic particles(SEPs) which is why there is another catalog associ-ating SEPs and radio bursts Thus Wind remainsan active partner in the CDAW Data Center

22 of 44

2017 Wind Senior Review Technical Implementation

Current Load Shed Setting [211 V]

Average BatteryTemperature [oC]

Regulated BusCurrent Output [A]

Minimum [Transmitter Off]Maximum [Transmitter On]Average

Wind Spacecraft Systems Status [Jan 1994 to Jan 2018]

Solar ArrayCurrent Output [A]

17Minimum [Mag Boom Shadow]Maximum [Non-Shadowed]

Average Battery BiasVoltage Output [V]

Battery 1Battery 2Battery 3

Year1995 1997 1999 2001 2003 2005 2007 2009 2011 2013 2015 2017

Figure 16 Summary of Windrsquos Status The Wind spacecraft systems status plotted from Jan 1 1994 to Jan1 2018 The figure shows the solar panel array (upper left) current [Amp] output regulated (upper right) buscurrent [Amp] average battery (lower left) temperatures [C] and average battery (lower right) bias voltage [Volts]versus time Each data point represents a daily average

5 Technical Implementation51 Spacecraft Health

Wind continues to operate in good health Thecommunication system was successfully reconfiguredin 2000 to enhance the telemetry margins and re-liance on a single digital tape recorder (with two tapeunits) since 1997 has never hindered operations Theflight operations team (FOT) took steps to minimizewear and extend the lifespan of the two tape unitsSince the last Senior Review the spacecraft has ex-perienced the usual instrument latch-ups and single-event upsets (SEUs) that are likely caused by highenergy particles As in the past the FOT was ableto restore all instruments to fully operational within aday or two depending on Deep Space Network (DSN)scheduling The automation of the recovery processfor the WAVES instrument after latch-ups (ie dueto SEUs) was successfully completed in October 2016and the spacecraft command tables now include au-tomated tests of the SWE electron instrument ThusWind continues to maintain a fully operational sta-tus

On Oct 27 2014 at 215938 GMT the Wind com-mand and attitude processor (CAP) suffered two si-multaneous SEUs The redundant nature of the Windspacecraft bus allowed the FOT to successfully switchto a second CAP CAP2 The FOT began the recov-

ery of CAP1 on Jan 21 2015 and finished Jan 302015 Thus the Wind spacecraft was fully recoveredat sim1750 UTC on Jan 30 2015

The CAP1 anomaly resulted in a complete loss ofdata from October 27 2014 until November 7 2014(ie 11 days or sim3 annual total) and partial lossfrom all instruments between November 7ndash20 2014(ie 14 days or sim4 annual total) The SWE in-strument suffered complete data loss between Octo-ber 27 2014 and November 26 2014 (ie 30 days orsim8 annual total) and partial loss (HK only) fromOctober 27 2014 to December 1 2014 (ie 35 daysor sim10 annual total) During the recovery processbetween Jan 28ndash30 2015 while CAP1 was in con-trol the attitudetelemetry information was invalidfor sim4 hrs 41 mins (ie lt5 of those four days)

An examination of the spacecraft power systems(see Figure 16) shows that the batteries can main-tain average bias voltages high enough to exceed the

23 of 44

current load shed setting of 211 V until at leastmid sim2027 (ie extrapolation to yellow line in lowerright-hand panel) To cause a spacecraft reset allthree batteries must simultaneously fall below thiscommandable voltage level The load shed setting iscommandable from ground and will be changed whennecessary to avoid a spacecraft reset We can safelyreduce the load shed setting down to at least 196 Vwhich corresponds to at least four more years (beyondsim2027) without issue

Since the last Senior Review all three batterieswent through two mode changes to reduce the maxi-mum charge voltage (see lower-left-hand panel in Fig-ure 16) Each battery was experiencing excess charg-ing causing an increase in temperature and reductionin efficiency The successful mode changes reducedthe temperatures to nominal ranges At least one ofthe three batteries will require another mode changein late sim2020 At this rate ndash sim3 years between modechanges ndash the batteries will last another sim15ndash18 yearssince there are currently 5 more mode levels availablebefore other alternatives are required

The solar array output is producing more thanenough current for spacecraft operations and will con-tinue to do so well past the year sim2018 assuming arequirement that a minimal current be drawn fromthe batteries (ie blue line in upper left-hand panelremains higher than red line in upper right) How-ever Wind operated for over a decade not satisfy-ing this requirement when in early 2012 a more effi-cient sequence of commands were implemented dur-ing transmission Under this less conservative re-quirement and the current rate of degradation thesolar arrays would no longer meet the minimum cur-rent requirements for the regulated bus output bythe late 2040rsquos (ie when the blue line in upper left-hand panel drops below the green line in upper right)Therefore Wind can operate at current capacity wellinto the next decade

Wind continues to maintain a large fuel reserveshowing sim54 kg remaining which is equivalent tosim103 ms of radial delta-V assuming normal thrusteroperations Wind need only perform sim4 station keep-ing maneuvers each year each of which only requiresim02ndash05 ms delta-V Thus Wind has enough fuelfor gt50 years

52 Instrument StatusSeven of the eight Wind instruments including all

of the fields and particles suits remain largely or fullyfunctional The only instrument turned off is theTGRS γ-ray instrument that was designed for onlya few years of operations The general status of allinstruments is summarized in Table 3

The specific degradations in instrument capabili-

ties are the following EPACT-IT detector failed andthe EPACT-APE detector only returns two energychannels of sim5 and sim20 MeV protons during en-hanced periods The LEMT and STEP telescopes ofthe same instrument continue to operate normallyproviding crucial and unique observations of solarenergetic particles up to 10 MeV in energy TheSMS-SWICS solar wind composition sensor had to beturned off in May 2000 The SMS DPU experienced alatch-up reset on 26 June 2009 that placed the MASSaccelerationdeceleration power supply into a fixedvoltage mode rather than stepping through a set ofvoltages It has been determined that a moderate riskpower cycling of the SMS DPU would be required tofix this problem In order to protect the unique andfully functional STICS sensor it has been decided toleave the MASS sensor in a fixed voltage mode thatallows reasonable but reduced science data collectionIn 2010 MASS experienced a small degradation inthe accelerationdeceleration power supply which re-duced the efficiency of the instrument though thisdoes not seriously affect science data analysis

The VEIS thermal electron detectors on the SWEinstrument experienced high voltage problems inNovember 2001 This problem was resolved by re-programming the SWE Strahl sensor to recover mostof the original functions Moreover the 3DP instru-ment also covers the impacted electron measurementsmaking these observations still redundant and hencerobust The entire SWE instrument suite required afull reset due to the CAP anomaly (see Section 51for details) which resulted in a complete loss of datafrom late Oct 27 2014 to Nov 26 2014 and par-tial loss until Dec 1 2014 when the instrument wasreturned to nominal operations

On May 2014 the 3DP instrument (specificallyPESA Low) suffered an anomaly that only affectedthe telemetry house keeping (HK) data A quickinvestigation showed that while the telemetry in-formation (eg micro-channel plate grid voltage)showed unreliable instrument operations informationthe science data remained unaffected (ie no notice-able change in flux was observed during and afterevent) All the other detectors within the 3DP in-strument suite continue to operate nominally Thusthe anomaly resulted in no loss of scientific data

Aside from the complete or partial data losses dueto the 2014 CAP and 2016 tape unit anomalies (seeSection 51 for details) all of the instruments con-tinue to be fully functional

53 Science TeamThe Wind instrumentscience team is very small

but an extremely dedicated group of scientists Dueto the longevity of the mission a number of the origi-

24 of 44

Table 3 The status of the Wind instrumentsInstrument Principal Investigator Institution Status

SWE AF- Vinas Electrons GSFC UNH Strahl detector reconfigured(acting) Ions SAO Faraday Cup fully operational

3DP SD Bale UC Berkeley Fully operationalMFI A Szabo GSFC Fully operational

SWICS turned offSMS S Lepri U Michigan MASS reduced coverage

STICS fully operationalEPACT LB Wilson III GSFC IT turned off

(acting) APE ndash only 5 and 20 MeV protonsLEMT and STEP operational

WAVES R MacDowall GSFC Fully operationalKONUS R Aptekar Ioffe Institute Russia Fully operationalTGRS B Teegarden GSFC Intentionally turned off

(ran out of coolant)

nal instrument PIs have retired or passed away KeithOgilvie passed the leadership of the SWE instrumentsuite to Adolfo Vinas (GSFC) and Justin Kasper(University of Michigan) leading the SWE FaradayCup team Stuart Bale has taken over as PI of 3DPat the University of California Berkeley Adam Sz-abo (GSFC) is the PI for the MFI instrument SueLepri (University of Michigan) is the PI for SMSBoth the original and previous acting EPACT PIsTycho von Rosenvinge and Allen Tylka respectivelyrecently retired so Lynn B Wilson III (GSFC) andJohn F Cooper (GSFC) are currently performing theduties of the EPACT PI until a suitable replacementcan be found Finally Dr Wilson was promotedto Project Scientist for Wind in June 2016 The newteam brings a great deal of experience and enthusiasmfor new discoveries as evidenced by the long and in-creasing list of Wind scientific publications (ie over600 refereed publications since the last Senior Re-view) There are also several new data sets that havebeen released since the last Senior Review and someto be released before the next Senior Review result-ing from efforts by the new team members (eg seeAppendix A)Students

Wind remains a very popular source of solar windmeasurements and a rich source of material for Mas-ters PhD and postdoctoral work Since the last Se-nior Review 13 students earned PhDs 3 studentsearned Masters degrees and 4 postdocs benefitedfrom Wind observations There are currently 16 PhDand 4 Masters students (of which we are aware) usingWind observations The university team membersalso rely on a large number of undergraduate internsto increase their scientific productivity

54 Ground OperationsWind ground operations take place at Goddard

and is fully transitioned from the legacy Polar -Wind -Geotail system to Multi-Mission Operations Center(MMOC) that consolidates Wind operations withthat of ACE This transition became necessary withthe decommissioning of Polar on April 30 2008 andit includes the upgrade of outdated and costly tomaintain hardware and software Wind operationswere moved to the MMOC on March 11 2010 withthe MMOC Operational Readiness Review held onMarch 30 2010

For cost saving measures the flight operationsteam reduced staffing by 1 FTE in November 2008and modified shift schedules to reduce operationalcoverage from twelve to eight hours (reducing theneed for overtime and shift differential) With thesuccessful transition of Wind flight operations intothe MMOC the staffing levels have been reduced tooperate the ACE and Wind missions with a combinedteam that also includes non-traditional flight opera-tions skills (HWSW maintenance Flight Dynamicsattitude analysis) Re-engineeringupgrading exist-ing systems promoted efficiency with respect to im-plementing IT Security and HW SW maintenance aswell as system administration Automation is beingimplemented with a unified approach to further in-crease efficiency (eg SWE electron instrument auto-recovery and WAVES recovery after latch ups) Theteams will continue to cross train at multiple posi-tions so that prime and backup roles are covered Inspite of the disruptions due to the 2014 CAP and 2016tape unit anomalies the data recovery rate for Windfor the years 2015 and 2016 averaged sim968 andsim984 respectively Since the recovery from the2016 TUA anomaly the median daily data recoveryrate has been gt99 Most of the unrecoverable data

25 of 44

2017 Wind Senior Review In-Guide Budget

loss occurred when Wind Deep Space Network (DSN)supports were released for other spacecraft launchesand emergencies with some data loss resulting alsofrom network problems

The current operation of Wind requires one sim2hour DSN support every other day though contactsoccur more frequently sometimes This allows the up-linking of the Stored Command Table load and theplayback of the Digital Tape Recorder (DTR) Windalso maintains real-time solar wind monitoring duringthese 2 hour contacts In 2001 an attempt was madeto reduce the number of DSN contacts and hence thecost of operations by scheduling DSN time only onceevery three days albeit for longer durations Reduc-ing the number of contacts saves the lengthy setupand reset times After extensive testing it was con-cluded that this scenario did not provide significantsavings and introduced critical risks to the missionWind can store only three days worth of commandsthus this is the longest Wind can go without groundcontact or the spacecraft performs an emergency loadshed Hence the current flexibility to negotiate con-tact time with DSN would be eliminated Also allof these infrequent contacts would be fully attendedregardless of the time of day Currently about halfof the contacts are completely automated allowingthe operation staff to keep day schedules Thus thecurrent daily contact scenario is considered optimalIt should be noted that all DSN and communicationcosts are reported as ldquoIn Kindrdquo costs so they are notconsidered part of Wind rsquos operational budget

The automated distribution and archiving of levelzero files and production of key parameter (KP) filestakes place at Goddard in the Science Directorate un-der the control of the project scientist The two server(plus backup) system are periodically upgraded andmaintained at modest cost

6 In-Guide Budget

The in-guide budget described in this section willfund the mission operations necessary to continue thesafe operation of the Wind spacecraft along with ba-sic data reduction and validation processes performedat the various instrument institutions As in pastSenior Reviews nearly all of the scientific researchoutlined in the previous sections are expected to beor were funded through external sources eg theROSES GI and SRampT programs (or other opportu-nities) with each element individually proposed andpeer reviewed The only funding allocated for scien-tific research in Wind rsquos budget occurs indirectly asa result of funding the instrument teams to processand validate the data

61 Mission Operations

The inputs in the budget spreadsheet Table 11show the direct and indirect costs for the Wind mis-sion The ldquoLaborrdquo line includes all civil servant la-bor dollars resulting from the ldquoFTE 1rdquo and ldquoFTE2rdquo lines The ldquoTravelrdquo line includes only traveldollars used by Code 670 for Wind -related meet-ingsconferences The ldquoMission Operationsrdquo sectionincludes all direct costs for flight operations and atti-tudeorbit support The ldquoData Analysisrdquo section in-cludes all costs funded directly through GSFC TheldquoTotal Uncostedrdquo section shows the expected eightweeks of uncosted carryover funds through the endof the fiscal year The last section shows ldquoIn-Kindrdquocosts that are indirect costs funded by other sourcesBelow we explain the costs included in each line ofthe budget spreadsheet

The total shown in the first line of the ldquoMission Op-erationsrdquo section includes the 56 WYEs for the FOT(ie ldquoWYE 1rdquo line) for FY18ndashFY22 It also includessupport from flight dynamics for orbit determinationand station keeping maneuvers and the DSN schedul-ing work The sustained engineering costs for FY18ndashFY22 are for system administration of the MMOCupdates to spacecraft commands hardware and soft-ware updates and level zero file processing The civilservant labor for a Mission Director (ie ldquoFTE 1rdquoline) is charged at 02 FTE and the dollar amount isincluded in the ldquoLaborrdquo line near the top

The ldquoData Analysisrdquo section includes all scienceoperations for the Wind project including on-site con-tractor labor (ie itemized in the ldquoWYE 2rdquo line)funding for a resource analyst at 02 WYE and all in-strument operations costs All civil servant labor dol-lars are not included here but shown in the ldquoLaborrdquoline near the top of the spreadsheet but are itemizedby time in the ldquoFTE 2rdquo line The totals for ldquoFTE 2rdquoinclude maintaining the Wind portion of the reengi-neered PWG system by a software engineer at 02FTE 05 FTE for the project scientist and 02 FTEfor data production and calibration split between theSWE (electron) and EPACT instruments The PWGsystem ndash responsible for the archival of the level zerodata and its distribution to the instrument sites andfor the generation of the quick-look key parameter(KP) data files ndash requires sim$30kyear for hardware(eg replacement hard drives) and software licensefees The remaining costs are distributed among theuniversity-led instrument teams Note that sim33 ofthe in-guide funding is needed for mission operationsand only sim6 for project management Thus morethan half of the Wind budget still goes to the in-strument teams for data processing and validationThe cost of the recent transition of the Wind pri-

26 of 44

mary recorder from tape unit A (TUA) to TUB willbe attempted to be absorbed in the existing smallfunding level

The ldquoIn-Kind costs to missionrdquo line includes ser-vices provided to Wind that are funded by othersources (eg SCAN) These costs are allocated toWind but are not supported with project funds Thisline includes costs for mission communication services(eg voice and data connections at GSFC) and sup-plemental costs for flight dynamics and flight oper-ations support The ldquoSpace Communications Ser-vicesrdquo line shows all DSN costs Again these costsare not supported with project funds

62 Data Production and AccessibilityThe Wind science data products are publicly

served directly from the instrument team sites (mostare directly available from CDAWeb) with a sin-gle project webpage containing links to and descrip-tions of the large number of Wind data products(httpswindnasagov) Wind is also an active par-ticipant in the development of the Virtual Helio-physics Observatory or VHO (httpsvhonasagov)that makes data queries even more user friendly andpowerful Details of the data production are givenbelow

Over half of the requested in-guide funding is al-located to the generation calibration and validationof the various Wind instrument data products Af-ter receiving the level zero instrument data alongwith housekeeping and ephemeris information theinstrument teams are responsible for the genera-tion of science quality data that is fully calibratedand validated typically through the performance ofwell established scientific analysis The instrumentteams are required to provide complete documenta-tion and intermediate-term archiving prior to finalsubmission to SPDFCDAWeb In addition the oc-casional (sim4year) station keeping maneuvers neces-sitate instrument level commanding that the instru-ment teams are required to support Thus besidesdata production expertise the teams have to main-tain a low level engineering capability that can sup-port routine and emergency operations Finally sinceWind does not have a project level science centerthe instrument teams are responsible for the pub-lic dissemination of their data through the main-tenance of local webpages and final submission toSPDFCDAWeb

Due to the limited funding available the in-strument teams optimized their processes to staywithin 1 FTE for all aspects of operation Allfully functional instruments (MFI SWEElectronSWEFaraday Cup WAVES 3DP and EPACT) areallocated nearly the same amount of support regard-

less of whether they are full cost accounted Goddardcivil service or university-led teams It should benoted that SWE is composed of two independent in-struments the Goddard electron instrument and theSAOUniversity of Michigan Faraday Cup

The SMS instrument team receives roughly half asmuch due to the reduced data production require-ments resulting from the SWICS failure early in themission and partial functioning of the MASS detec-tor (STICS is fully operational) However STICSstill continues to produce valuable and unique datatherefore continued support at this reduced level isstill requested The TGRS instrument was intention-ally turned off after it ran out of coolant (this was ex-pected and part of the design) thus has not receivedfunding for over 15 years Finally the astrophysi-cal KONUS instrument receives no heliophysics fund-ing This instrument receives some minor amountof funding in Russia for data production and evenless support from the Gamma-Ray Coordinates Net-work (GCN) ndash currently funded through High En-ergy Astrophysics Science Archive Research Center(HEASARC) ndash for minimal effort by a Goddard civilservant for data processing Thus no new fundingis requested for them in this proposal All of thesecosts except civil servant salaries are included in theldquoData Analysisrdquo section of Table 11

The current Wind project funding level does notallow any significant amount of funded science re-search and most of the results presented in this pro-posal were generated through independent funding(eg ROSES proposals) However the core data cal-ibration and validation work carried out by the indi-vidual instrument teams does require some amountof science data analysis to verify the accuracy ofthe generated data products It is difficult to bequantitative about the fraction of work involved inthis data validation work because it arises indirectlyfrom the calibration and validation of the instrumentdata However we can estimate an upper boundby summing the total labor costs for instrumentteam scientists-only (ie excluding overhead and en-gineertechnician and resource analyst salaries) find-ing that sim13 of the total Wind funding can be at-tributed to science data analysis or sim20 of the non-mission operations funding Again these are veryconservative estimates and all result indirectly fromthe normal calibration and validation of the instru-ment data

ReferencesAdrian M L et al (2016) Solar Wind Magnetic

Fluctuations and Electron Non-thermal Tempera-ture Anisotropy Survey of Wind-SWE-VEIS Ob-servations Astrophys J 833 49 doi103847

27 of 44

1538-4357833149Agueda N et al (2014) Release timescales of so-

lar energetic particles in the low corona Astronamp Astrophys 570 A5 doi1010510004-6361201423549

Altobelli N et al (2016) Flux and composition ofinterstellar dust at Saturn from Cassinirsquos CosmicDust Analyzer Science 352 312ndash318 doi101126scienceaac6397

Bale S D et al (2009) Magnetic FluctuationPower Near Proton Temperature Anisotropy In-stability Thresholds in the Solar Wind Phys RevLett 103 211101 doi101103PhysRevLett103211101

Bougeret J-L et al (1995) Waves The Radio andPlasma Wave Investigation on the Wind Space-craft Space Sci Rev 71 231ndash263 doi101007BF00751331

Burgess D et al (2012) Ion Acceleration at theEarthrsquos Bow Shock Space Sci Rev 173 5ndash47 doi101007s11214-012-9901-5

Chen C H K et al (2016) Multi-species Mea-surements of the Firehose and Mirror InstabilityThresholds in the Solar Wind Astrophys J Lett825 L26 doi1038472041-82058252L26

Dierckxsens M et al (2015) Relationship betweenSolar Energetic Particles and Properties of Flaresand CMEs Statistical Analysis of Solar Cycle 23Events Solar Phys 290 841ndash874 doi101007s11207-014-0641-4

Ebert R W et al (2012a) Corotating InteractionRegion Associated Suprathermal Helium Ion En-hancements at 1 AU Evidence for Local Accelera-tion at the Compression Region Trailing Edge As-trophys J 749 73 doi1010880004-637X749173

Ebert R W et al (2012b) Helium Ion Anisotropiesin Corotating Interaction Regions at 1 AU Astro-phys J Lett 754 L30 doi1010882041-82057542L30

Farrell W M et al (1995) A method of calibrat-ing magnetometers on a spinning spacecraft IEEETrans Mag 31 966ndash972 doi10110920364770

Fedorov A et al (2011) The IMPACT Solar WindElectron Analyzer (SWEA) Reconstruction of theSWEA Transmission Function by Numerical Sim-ulation and Data Analysis Space Sci Rev 16149ndash62 doi101007s11214-011-9788-6

Filwett R J et al (2017) Source Population andAcceleration Location of Suprathermal Heavy Ionsin Corotating Interaction Regions Astrophys Jin press

Fox N J et al (2016) The Solar ProbePlus Mission Humanityrsquos First Visit to Our

Star Space Sci Rev 204 7ndash48 doi101007s11214-015-0211-6

Gary S P et al (2016) Ion-driven instabilities inthe solar wind Wind observations of 19 March2005 J Geophys Res 121 30ndash41 doi1010022015JA021935

Gedalin M et al (2016) Dependence of the Spec-trum of Shock-Accelerated Ions on the Dynamicsat the Shock Crossing Phys Rev Lett 117 (27)275101 doi101103PhysRevLett117275101

Ghielmetti A G et al (1983) Calibration systemfor satellite and rocket-borne ion mass spectrom-eters in the energy range from 5 eVcharge to100 keVcharge Rev Sci Inst 54 425ndash436 doi10106311137411

Gloeckler G et al (1995) The Solar Wind andSuprathermal Ion Composition Investigation onthe Wind Spacecraft Space Sci Rev 71 79ndash124doi101007BF00751327

Greiner J et al (2015) A very luminous magnetar-powered supernova associated with an ultra-longγ-ray burst Nature 523 189ndash192 doi101038nature14579

Gruen E et al (1992) The ULYSSES dust experi-ment Astron amp Astrophys Suppl 92 411ndash423

Gruesbeck J R et al (2015) Evidence for Local Ac-celeration of Suprathermal Heavy Ion Observationsduring Interplanetary Coronal Mass Ejections As-trophys J 799 57 doi1010880004-637X799157

Hathaway D H (2015) The Solar Cycle Living RevSolar Phys 12 4 doi101007lrsp-2015-4

Jian L K et al (2016) Electromagnetic cyclotronwaves in the solar wind Wind observation andwave dispersion analysis in American Institute ofPhysics Conference Series American Institute ofPhysics Conference Series vol 1720 p 040007doi10106314943818

Kanekal S G et al (2016) Prompt acceleration ofmagnetospheric electrons to ultrarelativistic ener-gies by the 17 March 2015 interplanetary shockJ Geophys Res 121 7622ndash7635 doi1010022016JA022596

Kartavykh Y Y et al (2016) Simulation of Ener-getic Particle Transport and Acceleration at ShockWaves in a Focused Transport Model Implicationsfor Mixed Solar Particle Events Astrophys J 82024 doi1038470004-637X820124

Kasper J C (2002) Solar wind plasma Kineticproperties and micro- instabilities PhD the-sis MASSACHUSETTS INSTITUTE OF TECH-NOLOGY advisor Alan J Lazarus

Kasper J C et al (2006) Physics-based teststo identify the accuracy of solar wind ion mea-

28 of 44

surements A case study with the Wind FaradayCups J Geophys Res 111 3105 doi1010292005JA011442

Kasper J C et al (2008) Hot Solar-Wind He-lium Direct Evidence for Local Heating by Alfven-Cyclotron Dissipation Phys Rev Lett 101261103 doi101103PhysRevLett101261103

Kasper J C et al (2016) Solar Wind Electrons Al-phas and Protons (SWEAP) Investigation Designof the Solar Wind and Coronal Plasma InstrumentSuite for Solar Probe Plus Space Sci Rev 204131ndash186 doi101007s11214-015-0206-3

Kellogg P J et al (2016) Dust impact signals onthe wind spacecraft J Geophys Res 121 966ndash991 doi1010022015JA021124

Lepping R P et al (1995) The Wind MagneticField Investigation Space Sci Rev 71 207ndash229doi101007BF00751330

Lin R P et al (1995) A Three-Dimensional Plasmaand Energetic Particle Investigation for the WindSpacecraft Space Sci Rev 71 125ndash153 doi101007BF00751328

Lionello R et al (2014) Application of a SolarWind Model Driven by Turbulence Dissipation toa 2D Magnetic Field Configuration Astrophys J796 111 doi1010880004-637X7962111

Liu T Z et al (2016) Observations of a newforeshock region upstream of a foreshock bubblersquosshock Geophys Res Lett 43 4708ndash4715 doi1010022016GL068984

Malandraki O E et al (2012) Scientific Analysiswithin SEPServer ndash New Perspectives in Solar En-ergetic Particle Research The Case Study of the13 July 2005 Event Solar Phys 281 333ndash352 doi101007s11207-012-0164-9

Malaspina D M and L B Wilson III (2016) Adatabase of interplanetary and interstellar dust de-tected by the Wind spacecraft J Geophys Res121 9369ndash9377 doi1010022016JA023209

Malaspina D M et al (2014) Interplanetary andinterstellar dust observed by the WindWAVESelectric field instrument Geophys Res Lett 41266ndash272 doi1010022013GL058786

Maruca B A et al (2013) Collisional Thermal-ization of Hydrogen and Helium in Solar-WindPlasma Phys Rev Lett 111 (24) 241101 doi101103PhysRevLett111241101

Maruca B A et al (2016) Janus GraphicalSoftware for Analyzing In-Situ Measurements ofSolar-Wind Ions AGU Fall Meeting Abstracts ppSH11Andash2216 dec 12-16 2016 San Francisco CA

Matthaeus W H et al (2016) Ensemble Space-Time Correlation of Plasma Turbulence in the So-lar Wind Phys Rev Lett 116 (24) 245101 doi

101103PhysRevLett116245101McFadden J P et al (2008a) The THEMIS

ESA Plasma Instrument and In-flight Calibra-tion Space Sci Rev 141 277ndash302 doi101007s11214-008-9440-2

McFadden J P et al (2008b) THEMIS ESAFirst Science Results and Performance IssuesSpace Sci Rev 141 477ndash508 doi101007s11214-008-9433-1

Nieves-Chinchilla T et al (2016) A Circular-cylindrical Flux-rope Analytical Model for Mag-netic Clouds Astrophys J 823 27 doi1038470004-637X823127

Nieves-Chinchilla T et al (2017) Understandingthe internal magnetic field configurations of ICMEsusing 20+ years of Wind observations Solar Physsubmitted Feb 16 2017

Nitta N V et al (2015) Solar Sources of 3He-richSolar Energetic Particle Events in Solar Cycle 24Astrophys J 806 235 doi1010880004-637X8062235

Ogilvie K W et al (1995) SWE A ComprehensivePlasma Instrument for the Wind Spacecraft SpaceSci Rev 71 55ndash77 doi101007BF00751326

Omidi N and D G Sibeck (2007) Formation ofhot flow anomalies and solitary shocks J GeophysRes 112 A01203 doi1010292006JA011663

Reames D V (1999) Quiet-Time Spectra andAbundances of Energetic Particles During the 1996Solar Minimum Astrophys J 518 473ndash479 doi101086307255

Reames D V (2015) What Are the Sources of So-lar Energetic Particles Element Abundances andSource Plasma Temperatures Space Sci Rev 194303ndash327 doi101007s11214-015-0210-7

Reames D V (2016a) Temperature of the SourcePlasma in Gradual Solar Energetic ParticleEvents Solar Phys 291 911ndash930 doi101007s11207-016-0854-9

Reames D V (2016b) The Origin of ElementAbundance Variations in Solar Energetic Parti-cles Solar Phys 291 2099ndash2115 doi101007s11207-016-0942-x

Reames D V (2016c) Element Abundances andSource Plasma Temperatures of Solar EnergeticParticles in Journal of Physics Conference Se-ries J Phys Conf Ser vol 767 p 012023 doi1010881742-65967671012023

Reames D V and C K Ng (2001) On the Phase ofthe 27 Day Modulation of Anomalous and Galac-tic Cosmic Rays at 1 AU during Solar MinimumAstrophys J Lett 563 L179ndashL182 doi101086338654

Reames D V et al (2015) Temperature of the

29 of 44

Source Plasma for Impulsive Solar Energetic Par-ticles Solar Phys 290 1761ndash1774 doi101007s11207-015-0711-2

Richardson I G and H V Cane (2010) Interplan-etary circumstances of quasi-perpendicular inter-planetary shocks in 1996-2005 J Geophys Res115 7103 doi1010292009JA015039

Salas-Matamoros C and K-L Klein (2015) Onthe Statistical Relationship Between CME Speedand Soft X-Ray Flux and Fluence of the Asso-ciated Flare Solar Phys 290 1337ndash1353 doi101007s11207-015-0677-0

Stverak v et al (2008) Electron temperatureanisotropy constraints in the solar wind J Geo-phys Res 113 3103 doi1010292007JA012733

Suresh K and A Shanmugaraju (2015) Investiga-tion on Radio-Quiet and Radio-Loud Fast CMEsand Their Associated Flares During Solar Cy-cles 23 and 24 Solar Phys 290 875ndash889 doi101007s11207-014-0637-0

Tan L C and D V Reames (2016) Dropout ofDirectional Electron Intensities in Large Solar En-ergetic Particle Events Astrophys J 816 93 doi1038470004-637X816293

Turner D L et al (2013) First observationsof foreshock bubbles upstream of Earthrsquos bowshock Characteristics and comparisons to HFAsJ Geophys Res 118 1552ndash1570 doi101002jgra50198

Usmanov A V et al (2014) Three-fluid Three-dimensional Magnetohydrodynamic Solar WindModel with Eddy Viscosity and Turbulent Resistiv-ity Astrophys J 788 43 doi1010880004-637X788143

Vasanth V et al (2015) Investigation of the Geo-effectiveness of CMEs Associated with IP Type IIRadio Bursts Solar Phys 290 1815ndash1826 doi101007s11207-015-0713-0

Vinas A F et al (2015) Electromagnetic fluctu-ations of the whistler-cyclotron and firehose in-stabilities in a Maxwellian and Tsallis-kappa-likeplasma J Geophys Res 120 3307ndash3317 doi1010022014JA020554

von Rosenvinge T T et al (1995) The EnergeticParticles Acceleration Composition and Trans-port (EPACT) investigation on the WIND space-craft Space Sci Rev 71 155ndash206 doi101007BF00751329

Wang L et al (2015) Solar Wind sim20-200 keV Su-perhalo Electrons at Quiet Times Astrophys JLett 803 L2 doi1010882041-82058031L2

Wang L et al (2016) The injection often electron3He-rich SEP events Astron ampAstrophys 585 A119 doi1010510004-6361

201527270Weygand J M et al (2009) Anisotropy of the

Taylor scale and the correlation scale in plasmasheet and solar wind magnetic field fluctuationsJ Geophys Res 114 A07213 doi1010292008JA013766

Wicks R T et al (2016) A Proton-cyclotron WaveStorm Generated by Unstable Proton DistributionFunctions in the Solar Wind Astrophys J 819 (1)6 doi1038470004-637X81916

Wilson III L B (2016) Low frequency wavesat and upstream of collisionless shocks in Low-frequency Waves in Space Plasmas GeophysMonogr Ser vol 216 edited by A Keiling D-H Lee and V Nakariakov pp 269ndash291 Amer-ican Geophysical Union Washington DC doi1010029781119055006ch16

Wilson III L B et al (2013) Shocklets SLAMSand field-aligned ion beams in the terrestrial fore-shock J Geophys Res 118 (3) 957ndash966 doi1010292012JA018186

Wilson III L B et al (2016) Relativistic elec-trons produced by foreshock disturbances observedupstream of the Earthrsquos bow shock Phys RevLett 117 (21) 215101 doi101103PhysRevLett117215101 editorsrsquo Suggestion

Wood S R et al (2015) Hypervelocity dust im-pacts on the Wind spacecraft Correlations be-tween Ulysses and Wind interstellar dust detec-tions J Geophys Res 120 7121ndash7129 doi1010022015JA021463

Xu X et al (2015) Direct evidence for kinetic ef-fects associated with solar wind reconnection Na-ture Sci Rep 5 8080 doi101038srep08080

Yu W et al (2016) Small solar wind transientsat 1 AU STEREO observations (2007-2014) andcomparison with near-Earth wind results (1995-2014) J Geophys Res 121 5005ndash5024 doi1010022016JA022642

Zachilas L and A Gkana (2015) On the Vergeof a Grand Solar Minimum A Second Maun-der Minimum Solar Phys 290 1457ndash1477 doi101007s11207-015-0684-1

30 of 44

2017 Wind Senior Review Mission Archive Plan

A Mission Archive PlanEarly in its mission Wind and the other GGS spacecraft relied on a very capable and extensive science

operations center the Science Planning and Operations Facility (SPOF) The SPOF was responsible for thecollecting distribution and active archiving of all level zero (LZ) and ancillary data products The SPOFalso ran daily the instrument team provided data processing software to produce quick turnaround publiclyavailable data termed Key Parameters (KPs) The SPOF also provided science planning and softwaremaintenance services

With the passage of time and with reducing funding levels the SPOF had to be turned off and mostof its functions were passed on to the instrument teams and to a small operation the Polar -Wind -Geotail(PWG) system that continued to perform some LZ and KP functions This unavoidable decentralizationresulted in a degree of unevenness and disparity between the various Wind instrument data services Tosolve this problem key Wind instrument team members rallied around the new distributed Heliophysics DataEnvironment (HDE) concept and became funding members of the Virtual Heliospheric Observatory (VHO)The VHO provides a single point of entry for data location without the costly necessity of a dedicated scienceoperations center As a byproduct Wind instrument data were among the first to be fully documented withthe common SPASE dictionary based metadata standard thus providing the user community an even levelof descriptions of instruments and data productsMission Operations Center

Wind ground operations takes place at Goddard and is fully transitioned from the legacy system to Multi-Mission Operations Center (MMOC) that consolidates Wind operations with that of ACE This transitionbecame necessary with the decommissioning of Polar on April 30 2008 and it includes the upgrade ofoutdated and costly to maintain hardware and software Wind operations were moved to the MMOC onMarch 11 2010 and the MMOC Operational Readiness Review was held on March 30 2010

The primary responsibility of the MMOC is spacecraft commanding trend and anomaly analysis DSNscheduling the maintenance of Wind Near-Real-Time (NRT) passes and LZ generation for each instrumentand spacecraft housekeeping In addition the Goddard Flight Dynamics Facility provides orbit solutions tothe MMOC The MMOC in turn sends all of these data products daily to the PWG systemThe PWG System

The PWG system handles the active archiving of LZ and ancillary files and their distribution to theinstrument teams and various active archives The PWG system also performs the rapid KP data productionfor all instruments It resides at Goddard with the project scientist team The PWG system has beenstreamlined onto only two computers (a data server and a data processor with hot spares) and is fullyautomated to eliminate the need for data technicians The system is maintained by one civil service ITengineer at a fraction of an FTE This system also serves as the interface to the Wind NRT data streamwhich is real-time processed data during the daily sim2 hour long spacecraft telemetry contact times ThisNRT data is available in numerical and graphical format at httpspwggsfcnasagovwindnrt

The PWG system distributes the instrument and spacecraft housekeeping LZ files to the in-strument teams via FTP All of these LZ and orbitattitude files are also publicly accessible atftppwgdatagsfcnasagovpub Only the most recent 60 days are served in uncompressed format butthe whole mission is archived in GZip compression Even though the deep archival of these data files arehandled by SPDF the PWG system also backs up all LZ data at two physical locations and onto CDAWebIt should be noted that the whole Wind mission to date requires only sim400 GB of storage for the LZ dataso the backup requirements are not overwhelming

At the beginning of the mission all Wind instrument teams had to supply software to automaticallyprocess some portion of their data into science data products the KP data Even though the KP datais clearly not the highest quality data the instrument teams produce its quick release (within 24 hoursof observation) makes it a popular data product The PWG system maintains this software library withoccasional support (as needed) from the instrument teams and automatically places all the KP data onhttpscdawebgsfcnasagov A more detailed description of the various KP products is given at the instru-ment sections below

The PWG system also keeps the Satellite Situation Center (SSCWeb) up to date with orbit information(httpssscwebgsfcnasagov) Thus all orbit graphics generated on SSCWeb are always up to dateInstrument Data

The bulk of the instrument data dissemination takes place through CDAWeb that also serves as

31 of 44

the Wind Active Archive To aid the user community we also developed a Wind project webpage(httpswindnasagov) that identifies the entry point for each instrument data environment and providessome degree of common documentation The Wind project webpage includes an updated list of publicationsand a link to the Wind Wikipedia webpage (httpenwikipediaorgwikiWIND (spacecraft)) that we de-veloped Most of the Wind data products can also be searched down to the parameter level through VHOproviding rapid access to a wide range of events in the very long duration Wind data set Next we detailthe data product status of each Wind instrumentSWE Ions

Documentation The SWE Faraday Cup (FC) sub-system was designed to measure solar wind thermalprotons and positive ions The physical sensor is completely described in the Space Science Reviews articleOgilvie et al [1995] This article was also reproduced in the Global Geospace Mission book and portions of itare available through the Wind project webpage (httpswindnasagov) The data production proceduresare described by Ogilvie et al [1995] with a much more detailed discussion in Kasper [2002] Error analysisresults are included in each FC data file where systematic uncertainties of the measurements and calibrationagainst other Wind instruments are discussed in Kasper et al [2006] All of this information and is availableon the Wind project webpage

Data Products The PWG system on receipt of the LZ data immediately processes a KP data product forSWEFC This automated procedure uses a convected isotropic Maxwellian to fit to the reduced distributionfunctions collected by the FC These ASCII data files (92 s resolution) are available to the public within24 hours of the observations at CDAWeb (httpscdawebgsfcnasagov) While the KP products wereoriginally designed as browse quick look data the quality proved to be so high that this data productbecame a frequently used science level data product of the FC sub-system

A data production algorithm was developed that employs a bi-Maxwellian fit and obtains anisotropictemperatures for protons and a separate fit for Alpha particles The resulting data product (designated H1by CDAWeb) also contains the simpler moment computations primarily to allow direct comparison with theACE SWEPAM proton data The whole mission (ie late 1994 ndash Present) has been reprocessed with thisnew algorithm and is available generally till 2ndash3 months behind real time as it requires the final calibratedMFI magnetic field data that needs several months to be computed Finally the reduced velocity distributionfunctions (designated WI SW-ION-DIST SWE-FARADAY) for the two FCs were released as a data productfor the entire mission in March 2014 The details and documention for these data products can be foundWind project webpage (httpswindnasagov) and at CDAWeb (httpscdawebgsfcnasagov)

Table 4 Publicly Available SWE Ion Data ProductsData Product Cadence Coverage Format Location

KP Protons (K0) 92 s 19941117ndashPresent ASCII FTPHelpera

CDF CDAWebb

Bi-Maxwellian (H1) 92 s 19950101ndashPresentc CDF CDAWebReduced Velocity

Distributions 92 s 19941115ndash20140827d CDF CDAWeb(SW-ION-DIST)

a httpsftpbrowsergsfcnasagov b httpscdawebgsfcnasagov c sim6 month lag d range at time of submission

of proposal

It is also possible to obtain special proton beam fits on request from Michael Stevens (e-mail msteven-scfaharvardedu) at the Harvard Center for Astrophysics These fits are specialized in that they only treatevents where there is an extra proton beam in addition to the usual proton solar wind core and associatedalpha-particle beam The occurrence rate of such events is low enough to limit this data product on anevent-by-event basis However the availability of such a product is very important as it allows for tests ofionion instabilities

Finally Bennett Maruca released an open-source Python GUI ndash funded by NASA ROSES grants ndash calledJanus that allows users to interactively fit bi-Maxwellians for multiple (selectable) species to the reducedvelocity distributions The advantage of such software is that it can account for situations with multipleproton beams in addition to the alpha-particle population and even O6+ The software and documentationcan be found on GitHub at httpsgithubcomJanusWindFC

The list of publicly available data products are shown in Table 4 All of the FC data products are archived

32 of 44

at the SPDF active archiveSWE Electrons

Documentation The SWE electron sub-system consists of two electrostatic analyzers the vector spec-trometer (VEIS) and the Strahl spectrometer They were designed to measure the solar wind electrondistribution function The sensors are fully described by Ogilvie et al [1995] and the instrument descriptionportion of this paper can also be found at the Wind project webpage (httpswindnasagov)

Due to a high voltage supply failure the last available data from the VEIS detector is May 31 2001 Sincethe Strahl detector has very similar capabilities (though it was used in a different manner at the beginning ofthe mission) the spacecraft instrument and on-ground data processing software were rewritten to recover theelectron observations originally supplied by VEIS The SWE Space Science Reviews article has been updatedwith these modifications and is available at the Wind project page along with a technical description of thenew ground software algorithms Moreover the headers of the CDF data files have extensive documentationfor each data product

Data Products There are four SWE electron data products (1) electron moments from density to heatflux (2) pitch-angle distributions with 30 angle and 13 energy bins (3) reducedaveraged pitch-angle distri-bution data products and (4) strahl observations Starting on Aug 16 2002 all of these four data productsare generated by the new production software based on the reprogrammed Strahl detector measurementsIn addition the electron ldquomomentsrdquo are no longer the result of integral moment calculations but estimatedfrom the fitting of a single kappa distribution function to both the core and halo components

Table 5 Publicly Available SWE Electron Data ProductsData Product Cadence Coverage Format LocationMoments (H0) 6ndash12 s 19941229ndash20010531 CDF SPDF FTPa CDAWebb

Pitch-angle (H4) 12 s 19941130ndash20010710 CDF SPDF FTP CDAWebAvg Pitch-angle (M2) 12 s 19941228ndash20010710 CDF SPDF FTP CDAWeb

Strahl 12 s 19941229ndash20020814 binary SPDF FTPNew Moments (H5) 12-15 s 20020816ndash20170130c CDF SWEFTP CDAWeb

New Pitch-angle (H3) 12-15 s 20020816ndash20170130c CDF SWEFTP CDAWebNew Avg Pitch-angle (M0) 12-15 s 20020816ndash20170130c CDF SPDF FTP CDAWeba ftpspdfgsfcnasagovpub b httpscdawebgsfcnasagov c range at time of submission of proposal

Except for the Strahl data all electron data products are available through CDAWeb The strahl data isavailable from the instrument webpage (httpwebmiteduspacewwwwindwind datahtml) The cur-rent availability of the SWE electron data products is summarized Table 53DP

Documentation The Wind3DP instrument consists of six different sensors There are two electron(EESA) and two ion (PESA) electrostatic analyzers (ESAs) covering energies from sim5 eV to 30 keV andthree arrays of double-ended solid state telescopes (SST) for electrons (SST Foil) and ions (SST Open) forenergies sim25ndash500 keV and sim70ndash7000 keV respectively The ESAs measure the core solar wind and lowerenergy suprathermal particles while the SSTs are entirely focused on suprathermals The instrument is fullydescribed by Lin et al [1995] The instrument description portion of this paper is reproduced at the Windproject web site

The ESAs produce much larger volumes of data than can be telemetered to ground so theyrely heavily upon onboard processing and burst modes As a result a large number of 3DPdata products were developed some based on onboard processing and some generated on theground Some documentation of these data products exist at the 3DP instrument webpage(httpsprgsslberkeleyeduwind3dp) and more documentationnotes can be found on the UMN 3DPwebpage (httpsgithubcomlynnbwilsoniiiwind 3dp proswiki) Extensive 3DP metadata can also bepublicly located on VHO

Data Products As most Wind instruments 3DP team has provided a KP production software to be runautomatically at the PWG system This data product contains electron and ion fluxes at seven energies foreach particle and some basic moment computations and can be found at CDAWeb for the whole durationof the mission The rest of the data products include (1) onboard proton velocity moments (PM) with3s resolution (2) omnidirectional fluxes for thermal electrons (ELSP and EHSP) and ions (PLSP) (3)pitch-angle distributions for thermal electrons (ELPD and EHPD) and ions (PLPD) (4) omnidirectional

33 of 44

fluxes for suprathermal electrons (SFSP) and ions (SOSP) (5) pitch-angle distributions for suprathermalelectrons (SFPD) and ions (SOPD) (6) onboard electron velocity moments (EM not corrected for spacecraftpotential) and (7) nonlinear fits of electron velocity distributions (EMFITS E0 corrected for spacecraftpotential)

The publicly available data products are shown in Table 6

Table 6 Publicly Available 3DP Data ProductsData Product Cadence Coverage Format Location

K0 92 s 19941101ndash20170214j CDF CDAWeba

PMb 3 s 19941115ndash20161231j CDF CDAWeb Berkeleyc

ELSPd 24-98 s 19941115ndash20161231j CDF CDAWeb BerkeleyEHSPd 24-98 s 19941220ndash20161231j CDF CDAWeb BerkeleyPLSPd 24 s 19941115ndash20161231j CDF CDAWeb BerkeleyELPDd 24-98 s 19941115ndash20161231j CDF CDAWeb BerkeleyEHPDd 24-98 s 19941220ndash20161231j CDF CDAWeb Berkeley

SSTe SFSPf 12 s 19941115ndash20161231j CDF CDAWeb BerkeleySST SOSPf 12 s 19941115ndash20161231j CDF CDAWeb BerkeleySST SFPD 12 s 19941115ndash20161231j CDF CDAWeb BerkeleySST SOPD 12 s 19941115ndash20161231j CDF CDAWeb Berkeley

EMg 3 s 19941115ndash20161231j CDF CDAWeb BerkeleyEMFITS E0h 3ndash98i s 19950101ndash20041231j CDF CDAWeb Berkeley

a httpscdawebgsfcnasagov b onboard proton moments c httpsprgsslberkeleyeduwind3dpd E = electron P = proton L = low energy H = high energy SP = omni directional fluxes PD = pitch-anglee SST = solid state telescope f SF = foil (electrons) SO = open (protons) g onboard electron moments h corrected

and calibrated electron moments i varies depending on instrument mode j range at time of submission of proposal

New Data Products The current onboard electron moments (EM) suffer from effects of spacecraft charging(ie photoelectron contamination) Recent efforts have led to the creation of a new data product of electronvelocity moments (EMFITS E0) which have accounted for the spacecraft potential and calibrated againstthe upper hybrid line for total electron density The new data product has been released to SPDF anddistributed as CDF files for the entire mission It comprises electron velocity moments ndash from density toheat flux ndash derived from nonlinear fits of the entire velocity distribution covered by EESA Low and High(ie few eV to sim30 keV) at variable time resolutions depending upon instrument mode (eg sim3s resolutionin burst mode)

Future Data Products Bennett Maruca received funding to adapt his Janus software to analyze the PESALow and High velocity distributions A preliminary beta-version is expected to be released by the end ofcalendar year 2017

The 3DP team is currently working on a higher level data product that separates the three solar windelectron components ndash core halo and strahl ndash to produce a new publicly available dataset The datasetwould be similar to the EMFITS E0 data product but separate moments for each of the three electroncomponents The delayed release of this data product (ie relative to the EMFITS E0 data product) isdue to the complexities involved in re-calibrating the micro-channel plate efficiency and deadtime tablesfor both EESA Low and High in order to more accurately determine the true spacecraft potential Thesecalibrations do not significantly affect the total velocity moments but can be critical for accurate separationand characterization of the tenuous halo and strahl componentsSMS

Documentation The Wind SMS instrument suite is composed of three separate instruments theSupraThermal Ion Composition Spectrometer (STICS) the high resolution mass spectrometer (MASS)and the Solar Wind Ion Composition Spectrometer (SWICS) STICS determines mass mass per charge andenergy for ions in the energy range from sim6ndash230 keVe MASS determines elemental and isotopic abun-dances from sim05ndash12 keVe SWICS initially provided mass charge and energy for ions in the energy rangeof sim05-30 keVe but it failed early in the mission and was turned off in May 2000 thus produces no dataMASS has been in a fixed voltage mode since 26 June 2009 due to a DPU latch-up resulting in reducedscience output These instruments are fully described by Gloeckler et al [1995] The Instrument calibrationis fully described by Ghielmetti et al [1983] and in the PhD thesis of K Chotoo both available at the Wind

34 of 44

project page Additional data release notes are archived at the VHOData Products Until the failure of the SWICS instrument on May 27 2000 combined SWICS and STICS

KP files were generated that contain alpha particle information along with some carbon and oxygen abun-dances and temperatures This data product is still publicly available from CDAWeb The SWICS failureresulted in a significant effort to re-prioritize MASS and STICS A new software system was developed whichautomates many data analysis functions previously done manually The system first simultaneously assignsevents to specific ion species removing any overlap and using the statistical properties of the measurementsto maximum advantage It then uses these assigned events to construct phase space density distributionfunctions and corrects these for the effects of instrument efficiency and sampling geometry Finally it out-puts these distribution functions error estimates and count rates for each ion along with many intermediateproducts that facilitate detailed analysis The software can perform arbitrary time integrations of the dataand can optionally use an inversion method to remove overlap among ions in the instrument measurementspace

Daily averages of the proton and alpha particle phase space density distribution functions forthe whole mission is already publicly available through the Wind project webpage In additionhourly resolution STICS and MASS energy spectra for select days by request throughout the mis-sion are available in digital and graphical formats from the University of Michigan page (httpsolar-heliosphericenginumichedumission dbspectraphpcraft=2)

Table 7 Publicly Available SMS Data ProductsData Product Cadence Coverage Format Location

KP SWICS+STICS 4 hr 19941212ndash20000527 CDF CDAWeba

STICSb 1 day 19950101ndash20071231 ASCII Wind Projectc

SWICS+MASSd 1 hr Select Days ASCII UMichigane

STICSf 1 day 2005ndash2007 ASCII UMichigana httpscdawebgsfcnasagov b proton and alpha-particle distribution functions c httpswindnasagovd energy spectra e httpsolar-heliosphericenginumichedumission dbspectraphpcraft=2b omnidirectional proton and alpha-particle distribution functions

The publicly available data products are shown in Table 7Future Data Products The SMS team is currently working to release an enhanced STICS dataset for the

entire mission that will include full 3D distributions at 1 day 2 hour and adaptive (ie depends on countrates) time resolutions The ions that will be included in this new dataset are H+ He+ and He2+ C+ C5+and C6+ O+ O6+ and O7+ and Fe8+ Fe9+ Fe10+ Fe11+ Fe12+ Fe14+ and Fe16+ The dataset will alsoinclude the ratios O7+O6+ and C6+C5+ These data are completely unique to Wind and not currentlypublicly available The data will be released to SPDF as CDF filesEPACT

Documentation The Energetic Particles Acceleration Composition and Transport (EPACT) investiga-tion consists of multiple telescopes including the Low Energy Matrix Telescope (LEMT) SupraThermalEnergetic Particle telescope (STEP) and ELectron-Isotope TElescope system (ELITE) ELITE is composedof two Alpha-Proton-Electron (APE) telescopes and an Isotope Telescope (IT) IT failed early in the missionand was turned off while APE only returns two energy channels of sim5 and sim20 MeV protons during enhancedperiods LEMT ndash covering energies in the 1-10 MeVnuc range ndash and STEP ndash measuring ions heavier thanprotons in the 20 keV to sim1 MeVnuc range ndash still continue to provide valuable data These instrumentshave been described by von Rosenvinge et al [1995] The instrument portion of this paper is reproduced atthe Wind project webpage (httpswindnasagov) Additional instrument information is available at theinstrument webpage (httpsepact2gsfcnasagov)

Data Products Fluxes for a select number of ions (helium oxygen iron and combined CNO) in energybins below 1 MeVnuc and averaged over 92 seconds are publicly available for the whole mission in KP filesat CDAWeb However the low count rates of heavy ions leads to a significant fraction of this data productbeing null A systematic search for events with non-zero count rates was been undertaken where the teamidentified 41 multi-day duration periods of intense particle events in the 1997ndash2006 time range For theseintervals hourly omnidirectional intensity (OMN) ion sectored count (SEC) and first order ion anisotropydata were generated These ASCII text files are publicly available at the Wind project webpage

35 of 44

Table 8 Publicly Available EPACT Data ProductsData Product Cadence Coverage Format Location

KP fluxes 92 s 19941116ndash20170214h CDF CDAWeba

OMNb 1 hr 41 Events ASCII Wind Projectc

SECd 1 hr 41 Events ASCII Wind ProjectAnisotropy 1 hr 39 Events ASCII Wind Project

LEMTf 1 hr 19941103ndash20161231h CDF CDAWebLEMTf 5 min 19941103ndash20140906h CDF CDAWebAPE-Bf 1 hr 19941103ndash20161231h ASCII VEPOg

a httpscdawebgsfcnasagov b omnidirectional fluxes c httpswindnasagov d sectored countse httpsomniwebgsfcnasagov f omnidirectional fluxes g httpsvepogsfcnasagovh range at time of submission of proposal

Hourly-averaged omnidirectional particles fluxes from LEMT subsystem of the WindEPACT instrumentare available from OMNIWeb (httpsomniwebgsfcnasagov) and SPDFCDAWeb The data cover theentire mission from 3 November 1994 ndash 31 December 2016 and will be updated periodically These dataare also available at the Virtual Energetic Particle Observatory or VEPO (httpsvepogsfcnasagov) Thedata include He C O Ne Si and Fe in seven energy bins (six for Ne) from sim2ndash10 MeVnuc The MultindashSource Spectra Plot Interface of VEPO allows one to easily compare simultaneous measurements from othermissions (eg ACE STEREO etc) Locations of the LEMT data can be found in the Heliophysics DataPortal or HDP (httpheliophysicsdatascigsfcnasagov) using the text restriction rdquoLEMTrdquo

Future Data Products The EPACT team is working to produce data from the STEP telescope for theentire mission The data product will include 1 hour sector-averaged and 10 min omnidirectional intensitiesbetween sim20ndash2560 keVnuc in sim6ndash10 energy steps The heavy ions included in this dataset will include HHe CNO NeS and Fe Similar to the new SMS data products this will be unique to WindMFI

Documentation The Wind Magnetic Field Investigation (MFI) is composed of two fluxgate magnetometerslocated at the mid point and end of a long boom The instrument measures DC vector magnetic fields upto a time resolution of sim22 or sim11 vectorssec depending on the telemetry mode of the spacecraft Theinstrument is completely described in an article by Lepping et al [1995] The instrument description sectionsof this paper are reproduced at the Wind project webpage (httpswindnasagov) The data processingalgorithms employed in generating the MFI data products are described by Farrell et al [1995] available atthe Wind Project webpage

Data Products The MFI team generates 3-vector magnetic fields at multiple time resolutions (eg 3s 92setc) with varying calibration qualities depending on the data product Within 24 hours of measurement the92-second KP data is publicly available at CDAWeb This data uses periodically updated calibration tablesGenerally within sim1ndash2 weeks the MFI team produces a calibrated data product that includes 3-second 1minute and 1 hour averages (version 3) Roughly one month after measurement the final calibration andoffsets are determined with uncertainties now reduced to a few tenths of a nT (version 4) The version 4 CDFfiles replace the version 3 files when uploaded to SPDFCDAWeb The final archival data product (version5) requires sim2ndash3 months to remove all spacecraft ldquonoiserdquo and other artifacts All of these file versions havethe exact same internal format

Table 9 Publicly Available MFI Data ProductsData Product Cadence Coverage Format Location

KP 92 s 20100901ndash20170214a CDF CDAWebb

Versions 3 amp 4c 3 s 1 min 1 hr 19941116ndash20170209a CDF CDAWebVersion 5 (H0) 3 s 1 min 1 hr 19941116ndash20170209a CDF CDAWebHigh Res (H2) sim11 or sim22 vecsec 19941116ndash20170209a CDF CDAWeb

a range at time of submission of proposal b httpscdawebgsfcnasagov c files are eventually replaced by version

5 and no longer publicly available

The publicly available data products are shown in Table 9The highest sample rate data (ie sim11 or sim22 vectorssec depending on spacecraft location relative to

Earth) is kept in a separate CDF file (H2) from the lower rate data (H0) at sim3s resolution This is partly

36 of 44

due to file size differences backwards compatibility (ie the sim11 vectorssec was never included in the H0files) and differences in calibration efforts (eg spin tones and other effects not present in H0 data)WAVES

Documentation The Wind WAVES experiment is composed of three pairs of orthogonal antennas (electricfields) and a search coil magnetometer that operate as both radio receivers from simfew Hz to sim13 MHz andburst waveform capture time series receivers The radio receiver array includes the low frequency FFTreceiver (FFT) from simfew Hz to sim11 kHz the thermal noise receiver (TNR) from sim4 kHz to sim256 kHzradio receiver band 1 (RAD1) from sim20 kHz to sim1040 kHz and radio receiver band 2 (RAD2) sim1075ndash13825MHz The waveform capture array contains two time domain sampler (TDS) receivers slow (TDSS) and fast(TDSF) The TDSS receiver returns four vector fields of three magnetic(electric) and one electric(magnetic)field components at sample rates from sim117ndash7500 vectorss The TDSF receiver returns two electric fieldcomponents at sample rates from sim1800ndash120000 vectorss The instrument is fully documented by Bougeretet al [1995] The instrument related sections of this paper are reproduced at the Wind project webpage(httpswindnasagov) Some additional documentation exists also at the WAVES instrument webpage(httpssolar-radiogsfcnasagovwindindexhtml) The content and format of the various WAVES dataproducts are also described on the instrument webpage

Data Products As most other Wind instruments WAVES also produces a KP data product that is imme-diately publicly available at CDAWeb The WAVES KP data contains 3-minute averages of the electric fieldintensities at 76 log-spaced frequencies and electron density estimates based on neural network determinedelectron plasma frequency values The WAVES team produces 1 min resolution radio data within sim1 weekof observation as a frequency vs time intensity product and distributes these data on both the instrumentwebpage and CDAWeb The sim7ndash10 second total electron density estimates from the upper hybrid line arealso made available on CDAWeb

The WAVES team also maintains a Type IIIV catalog on the instrument website and a similar list can befound at the CDAW Data Center (httpscdawgsfcnasagovCME listradiowaves type2html) or througha link on the Wind project webpage

Table 10 Publicly Available WAVES Data ProductsData Product Cadence Coverage Format Location

KP 3 min 19941110ndash20170214g CDF CDAWeba

TNRb Rad1 Rad2c 1 min 19941110ndash20170214g ASCII IDL Save CDAWeb WAVESd

High Res nee 7-10 s 19941110ndash20170215g CDF CDAWeb

Radio Plots 1 min 19941110ndash20170215g PNG PDF WAVESDust Impactsf NA 19950101ndash20151231 CDF CDAWeb

a httpscdawebgsfcnasagov b Thermal Noise Receiver c Radio Receiver Band 1 2d httpssolar-radiogsfcnasagovwindindexhtml e electron number density f dust impact databaseg range at time of submission of proposal

The publicly available data products are shown in Table 10New Data Products A recently available product is the dust impact database produced by David

Malaspina (PI) and Lynn B Wilson III (Co-I) for the WAVESndashTDSF waveform captures The databaseis publicly available on CDAWeb in CDF file format The dataset includes the date and time orientationand location of the spacecraft impact location on the spacecraft body dust signal type etc The details ofthe dataset are described in Malaspina and Wilson III [2016] and very detailed metadata can be found atCDAWeb

Future Data Products The WAVES team is nearly ready to release all TDSS and TDSF events for theentire mission for final archive to SPDFCDAWeb The data products will be provided in CDF format andreleased for public use on CDAWeb The team has already produced a first version of the data product withsuccessful test results for ISTP (International Solar-Terrestrial Physics) compatibility from the SPDF teamThe WAVES team is currently finalizing the software for automated productionKONUS and TGRS

The KONUS and TGRS γ-ray instruments are not maintained by heliophysics Their data productionand data distribution is completely handled by the astrophysics division Description of the instruments andlinks to their data products can be found athttpsheasarcgsfcnasagovdocsheasarcmissionswindhtml and

37 of 44

httpsheasarcgsfcnasagovw3browseallipngrbhtmlWind and VHO

Members of the Wind instrument teams have taken leadership roles in the development of the VirtualHeliospheric Observatory (VHO) (httpsvhonasagov) Aside from assuring that the various data productsare publicly open the most effort went into the generation of SPASE dictionary based and VHO compliantmetadata In fact the first Wind data product metadata files have been used to refine the SPASE dictionaryfor fields and particles data Currently all primary Wind data products are fully searchable via the VHO

38 of 44

2017 Wind Senior Review Acronyms and Initialisms

Acronyms and Initialisms3D three-dimensional

3DP Three-Dimensional Plasma and Energetic Particle Investigation (Wind3DP)

ACE Advanced Composition Explorer

ACR Anomalous Cosmic Ray

APE Alpha-Proton-Electron telescope (part of Wind EPACTELITE)

ARTEMIS Acceleration Reconnection Turbulence and Electrodynamics of the Moonrsquos In-teraction with the Sun

AU Astronomical Unit

CAP Command and Attitude Processor

CCMC Coordinated Community Modeling Center

CDAWeb Coordinated Data Analysis Web

CIR Corotating Interaction Region

CME Coronal Mass Ejection

CRIS Cosmic-Ray Isotope Spectrometer

DiP Distortion Parameter

DSA Diffusive Shock Acceleration

DSCOVR Deep Space Climate Observatory

DSN Deep Space Network

DTR Digital Tape Recorder

EPO Education and Public Outreach

EESA Electron Electrostatic Analyzer (Wind3DP)

EH Electron Hole

ELITE Electron-Isotope Telescope system (WindEPACT)

EPACT Energetic Particles Acceleration Composition and Transport (APE-ELITE-IT-LEMT package on Wind)

EPAM Electron Proton and Alpha Monitor

EPP Electron Pitch-angle distribution Parameter

ESA (agency) European Space Agency

ESA (detector) Electrostatic Analyzer

ESW Electrostatic Solitary Wave

FAB Field-Aligned (ion) Beam

39 of 44

FC Faraday Cup

FOT Flight Operations Team

FR Flux-Rope

FTE Full Time Equivalent

FTP File Transfer Protocol

GCN Gamma-ray Coordinates Network

GeV Giga-electron volt

GF Giant Flare

GGS Global Geospace Science

GLE Ground-Level Events

GOES Geostationary Operational Environmental Satellites

GRB Gamma Ray Burst

GSFC Goddard Space Flight Center

GUI Graphical User Interface

HDP Heliophysics Data Portal

HET High-Energy Telescope

HETE-2 High Energy Transient Explorer-2

HGO Heliophysics Great Observatory

HI Heliospheric Imagers

HK House Keeping

HSO Heliophysics System Observatory

HTR High Time Resolution

IBEX Interstellar Boundary Explorer

ICME Interplanetary Coronal Mass Ejection

ICW Ion Cyclotron Wave

IMAP Interstellar MApping Probe

IMF Interplanetary Magnetic Field

IMP Interplanetary Monitoring Platform (spacecraft)

IMPACT In-situ Measurements of Particles and CME Transients (suite)

INTEGRAL INTErnational Gamma-Ray Astrophysics Laboratory

IP Interplanetary

IPD Interplanetary Dust

40 of 44

IPM Interplanetary Medium

IPN Interplanetary GRB Network

ISD Interstellar Dust

ISS International Space Station

ISTP International Solar-Terrestrial Physics

iSWA integrated Space Weather Analysis system

IT (detector) Isotope Telescope (part of Wind EPACTELITE)

ITOS Integrated Test and Operations System

keV kilo-electron volt

KH Kelvin-Helmholtz

KONUS Gamma-Ray Spectrometer

KP Key Parameter

LASCO Large Angle and Spectrometric COronagraph

LEMT Low Energy Matrix Telescopes (WindEPACT)

LET Low Energy Telescope

LIGO Laser Interferometer Gravitational-Wave Observatory

LWS Living With a Star

LZ Level Zero

MAG magnetic field experiment

MASS high-resolution mass spectrometer (WindSMS)

MAVEN Mars Atmosphere and Volatile EvolutioN mission

MC Magnetic Cloud

MESSENGER Mercury Surface Space Environment Geochemistry and Ranging

MeV Mega-electron volt

MHD Magnetohydrodynamic

MMOC Multi-Mission Operations Center

MMS Magnetospheric Multi-Scale NASA STP mission

MO Magnetic Obstacle

MOMS Mission Operations and Mission Services

MOVE Mission Operations Voice Enhancement

NASA National Aeronautics and Space Administration

OMNI omnidirectional or dataset on CDAWeb

41 of 44

PAD Pitch-Angle Distribution

PESA Ion Electrostatic Analyzer (Wind3DP)

PLASTIC PLAsma and SupraThermal Ion Composition

PMS Planar Magnetic Structure

PWG Polar-Wind-Geotail ground system

RBSP Radiation Belt Storm Probes (now Van Allen Probes)

RHESSI Reuven Ramaty High Energy Solar Spectroscopic Imager

SC Solar Cycle

SDO Solar Dynamics Observatory

SECCHI Sun-Earth Connection Coronal and Heliospheric Investigation

SEP Solar Energetic Particle

SEPT Solar Electron and Proton Telescope

SEU Single Event Upset

SGR Soft Gamma Repeater

SHH soft-to-hard-to-harder (ie change for X-ray spectra)

SIR Stream Interaction Region

SIS Solar Isotope Spectrometer

SIT Suprathermal Ion Telescope

SLAMS Short Large Amplitude Magnetic Structures

SMD Science Mission Directorate

SMS Solar Wind and Suprathermal Ion Composition Experiment (SWICS-MASS-STICS package on Wind)

SOHO SOlar and Heliospheric Observatory

SolO Solar Orbiter mission

SPASE Space Physics Archive Search and Extract

SPDF Space Physics Data Facility

SPP Solar Probe Plus mission

sps samples per second

SSMO Space Science Mission Operations

SSN Sun Spot Number

SST Solid-State (semi-conductor detector) Telescope (Wind3DP)

ST Small Transient

STE SupraThermal Electron instrument

42 of 44

STEP SupraThermal Energetic Particle Telescope (WindEPACT)

STEREO Solar-Terrestrial Relations Observatory

STICS SupraThermal Ion Composition Spectrometer (WindSMS)

SWE Solar Wind Experiment

SWEA Solar Wind Electron Analyzer

SWEPAM Solar Wind Electron Proton Alpha Monitor (ACE)

SWICS Solar Wind Ion Composition Spectrometer

SWIMS Solar Wind Ion Mass Spectrometer

TD Tangential Discontinuity

TDS Time Domain Sampler (WindWAVES)

TDSF Time Domain Sampler Fast (WindWAVES)

TDSS Time Domain Sampler Slow (WindWAVES)

TGRS Transient Gamma-Ray Spectrometer

THEMIS Time History of Events and Macroscale Interactions during Substorms

THOR Turbulence Heating ObserveR

TNR Thermal Noise Receiver (eg part of WindWAVES)

TPOCC Transportable Payload Operations Control Center

TRACE Transition Region And Coronal Explorer

TUA Tape Unit A

TUB Tape Unit B

ULEIS Ultra Low Energy Isotope Spectrometer

VDS VoiceVideo Distribution System

VEIS Vector Ion-Electron Spectrometers (WindSWE)

VEPO Virtual Energetic Particle Observatory

VEX Venus EXpress

VHO Virtual Heliophysics Observatory

VWO Virtual Waves Observatory

WYE Work Year Equivalent

43 of 44

2017 Wind Senior Review Budget Spreadsheet

Budget Spreadsheet

Table 11 Wind Senior Review Budget Spreadsheet

44 of 44

Executive Summary

Science and Science Implementation

Historical Background

Current Status

Winds Unique Capabilities

Heliophysics System Observatory

Prior Prioritized Science Goals

PSG 1 Two Full Solar Cycles

PSG 2 Solar Wind Structures

PSG 3 Kinetic Physics

PSG 4 Dust Science

Noteworthy Studies

New Prioritized Science Goals

Field-Particle Studies

Unusual Solar Cycle

Particle Acceleration

Long-Term Dust Science

Wind in the Heliophysics System Observatory

Wind and ACE DSCOVR STEREO and MAVEN

Wind and Solar Probe Plus and Solar Orbiter

Wind and IBEX and Voyager

Wind and Van Allen Probes MMS THEMIS and Cluster

Solar and Astrophysics

Wind CCMC and CDAW Data Center

Technical Implementation

Spacecraft Health

Instrument Status

Science Team

Ground Operations

In-Guide Budget

Mission Operations

Data Production and Accessibility

References

Mission Archive Plan

Acronyms and Initialisms

Budget Spreadsheet