1970 Solar Eclipse Press Kit

8/7/2019 1970 Solar Eclipse Press Kit

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NATIONAL AERONAUTICS AND'SPACE, ADMINISTRATION WO 24155

WASHINGTON,D .C . 20546 WO 3-925

FOR, RELEASE: SUNJD'AY

March 1,. 1970

RELEASE NO: 70-28

PROJECT: 1970 SOLAR ECLIPSE

contents

GENERAL RELEASE-----------------------------------------------1-7-

IWALLOPS ISLAND SOUNDING ROCKETS--.---------------------------8-13

LAUNCH VEHICLES-- .--------------------------------------- 14-17

SCIENTIFIC EXPER.IMENTS ------------------- --------- 8) M eteoro logy ----------------------------------------------18-21

Ionospheric Ph ysics-------------------------------------22-25

Solar Phy~sics ..,------ 2-------------5-

WALLOP, RANGE OPERATIONS ------------------------- ---- ?---8-29

WHITE SANDS MIS-SILE-RANGE SOUNDING ROCKETS-------------------30-31

SATELLITE AND.SPACE PROBE OBSERVATIONS-----------------------32-314

GROUND OBSERVATIONS------------------------------------------35-39

K.

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2/20 /70



E-NATIONAL AEONAUTICSAND SPCE AMINISTTRATION (20) 9-g4155

NEWSSHTO14D.J 205* TEOS: 2(202 9392

FOR RELEASE: SUNDAYMarch 1, 1970.

RELEASE 'NO:' 70-28

1970 SOLAR ECLIPSE,

Using-spacecraf-t in-deep- space, Earth orbital sate1-1ites,.

sounding rocke'vs and instruments on-'the ground', scientists will

make, ani intense 'study of the 1970 e.clipse of-the Sun on-March 7,.

concentra'ting on the effect the fairly abrupt and brie-f cessati-on

of sunlight will have-on Earth's atmosphere.

'The bulk -of the experiments sponsoreduby ,the National

Aeronautics and Space Administration will observe eclipse effects

on theEarth's atmosphere and ionosphere but some.will s'tudy 'the

'Sun itself with observations only possible- when .the, isko the

Sun is occulted by the 'Moon-.

Highlight of the NASA-sponsored studies will, be .the, aunch-

irig of 32 sounding rockets from its Wallops Station, Va.,.,f'acility

including,26.onthe day of the eclipse.

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2/20/7'



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Two other sounding rocket experiments will be launched

from the White Sands Missile Range, N.M.., outside the path of

the ecl-ipse to gather comparative data for 'the Wdilops flights.

A study of effects of the eclipse will be made with radio

signals from Mariner 6, over a distance of 235.,millihon miles from

Earth on the opposite6 sIde of the- Sun. Six Earth-orbiting

satellites al-so wiJ3.1 observe the eclipse' and its effects --

Orbiting Solar Observatorles 5 and 6, Applications Technology.

'S'atellite -3, nd three U...S./CaQnnadian satellites, Alouettes. 1 and,

*2 nd- International Satelllte for-Ionospheric Studies l1

The two OS. spacecraft will .use their ability to, point

instruments at the Sun 'to gather a large amount of data on-the

Sun and its atmospheire. ATS' wili photograph t,he Earth and its

cloud cover duri-ngtotality to bbserve the path of eclipse across

the-eastern United'States. The Canadianzsatellites w'ill investigate

eclipse-caused changesi'n the ionosphere Sfrom above.,

On the ground, NASA-sponsored obseravationrs wili be made of'

the eclipse f~rom threc locations, two-in Virginia and one in

Mexico.

The maximum eclipse at Wallops, -when the Sun will be

,almost totally obscured, will occur at 1:38 p.m.'ESTj March 7

.and will last for approximately three minutes.

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The neart otality of the eclipse at Wallops plus the

'large number of rocket launches are expected to attract a

A great number of people to the area. In cooperation.with

Wallops Station, the. National Park Service has established

a viewing site for the public near the, south end of

As'sateague Island. The site can be reached, by turning east

* off U.S. 13- onto Virginia Route. 175, traveling 13. miles

through the- town -of Chincoteague, to. the site.

Warnings about eye damage from wat.ching the eclipse have

been issued by the American Association of Opthalmology and

,the NationalSo'cietyf6r the Preventi-oh of'Blindness.

The organizatiOns say damage to the eyes from eclipsee-

watching involves burning the retina, and it is difficult to

*tell when.such damage. is occurihg because the retina is in-. C

seisitive to- pain.

The damage produces a blank spot in the field of vision

at the vital area ofLthe retina used for reading and fine

seeing. The damage is permanent -- incurable.,

No sunglasses, smoked glass, or photographic film is

absolutely safe.Though they may eliminate the glare of the

visible light, they do not block infrared rays which cause

damaging burns.

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-- 4-

The American-Association of' Opthalmology advises

watching.the image of the;eclipse by using za pinhole

device. This involves usingt~wo pieces of white card-

board with a pinhole in the top cardboard which projects

and focuses the image onthe second cardboard. The size

of the image may be changed by-altering the distance

between--the cardboards. Thus the observer can- view the

eclipse with his back to the Sun..

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This is not the first tinme that sounding rockets have

been used to study an eclipse. in May, 19-66, five sounding

-ockets were launched from the Wallops telemetry ship, Range

Recoverer, in the Mediterranean Sea near Greece. Fifteen

sounding rockets were launched in a joint U.S./Brazil program

from the southeast corner of Brazil in November 1966.

The effect of a solar eclipse is not uniform at all

altitudes above Earth so a variety of studies at various

altitudes are required.

Scientific investigations will be made in three disciplines

-- meteorology, ionospheric physics and solar physics. Eleven

research organizations including four universities will conduct

the experiments.

Six types of sounding rockets will be-used -- Arcas, Nike-

Apache and Nike-Cajun, Nike-Tomahawk and Nike-Iroquois, Aerobee

150, Aerobee 170, and Javelin. The Javelin is a four-stage

solid-fuel rocket and Wiil be the largest in the series. The

Aerobee 170 is a new configuration consisting of the reliable

Aerobee 150 sustainer and Nike booster which was test launched

on February 5 and 13.

For the 1970 eclipse, Wallops is augmenting its launching,

tracking and data acquisition capabilities to allow the large

number of scientific payloads to be launched in such a short

period.

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-6-

The firing schedule calls for some rockets to be fired

within a few seconds of each other, so Wallops has established

six launch areas with additional launchers set up at several

of those areas. Six mobile radars have been set up to augment

seven large radars at permanent sites. Five mobile telemetry

vans and the Wallops telemetry ship, Range Recoverer, will

assist the permanent multiple telemetry station.

Two payloads, solar physics experiments aboard the two

Aerobee rockets, will be recovered at.sea by Navy and Coast

Guard ships. Recovery is also nned for the two experiments

to be launched at White Sands.

The overall Unite'- States 1970 eclipse study is being

coordinated by the Nation-l Science Foundation. Dr. Albert E-.-

Belon is U.S. eclipse coordinator.

For NASA, the eclipse study is under direction of the

Office of Space Science and Applications with support from the

Office of Tracking and Data Acquisition. NASA eclipse coordinator , .

is Dr. Goetz K. Oertel.

For the Wallops sounding rocket project, NASA program

manager is Peter Eaton. For Wallops, the project manager is

Cary Milliner. For the Goddard Space Flight Center, vehicle

coordinators are Karl R. Medrow and George E. MacVeigh.

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Fcril the Lfank.ey Research Center, the eclipse coordinator is

I'avid Adniraonn, Space -Physics Brancrh, Aerophysics Division.

HNI.) OF RfELEASE1; BACKGROUND :NFORMATION FOLLOWS

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WALLOPS ISLAND 'SOUNDING ROCKETS

An unprecedented number of sounding rockets to study

the 1970 solar eclipse will be fired from the Wallops Island

launching area of NASA's Wallops Station.

Preliminary planning for the project started in March

1969. The first meeting of major-experimenters was held in

'September.. During the fall of 1969, installation of tempo-

rary power units, communications systems, radar units, ad-

ditional launchers and firing control circuits was completed.

Launch operation centers and payload preparation areas were

completed in February.

During the period of the eclipse launches, there Fi11 be

one launch unrelated to the eclipse, a Nike-Cajun rock tfrom

Launch Area 5 at 12:29 p.m. on March 8 carryinga-meteo

logical grenade experiment.

There follows a schedule of the sounding rockets to be

launched to make eclipse studies.

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WALLOPS

STAT ION

PRESS SITE. and

PUBLIC BLEACHERtsI

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WALLOPS ISLAND.ECLIPSE'LAUNCH 'SCHEDULE

NOTES: This schedule is subject to last-minute changes.

BU: backup. o be launched only iff.previous launch of same experiment fails.

ARCAS launches Will be from Area 2A, 500 feet' north aoaunch jArea 2.

NO. LAUNCH TIME LAUNCH AREA VEHICLE , EXPERIMENT, -,-EXPERIMENTERS,

Friday, March 6

1 4:30 a.m. 5 Nike-Cajun Meteorology-ozone, Godda4d Space Flight

water vapor Center

2 12:20 p.m.2A ARCAS Meteorology Langley Research

Center/EnvironmentalScience Services

Administration

3 1:24 p.m. 5 Nike-Apache Metelorol6gy-pitot Goddard-Space Flight-

probe Center/University of

Michigcn

4 1:36 p.m. 3 Nike-Apache Ionospheric physics- GCA Corp./Lockheed

solar X-rays Miss'iles & Space Co.

Saturdasr, March 7

5 9:30 a.m. 2A ARECAS Meteorology Langley Research

Center/Ehvironmental'Science Services

Administration'

6 10:45 a.m. 2 Nike-Apache Ionospheric physics- University of Illinois

radio\propagat ionelectr measurements

7 11:00 a.m. 2A ARCAS Mete6rboiy Langley Research

Center/Environmental

Science Serviqes

Administration

/,



NO. LAUNCL AREA VEHICLE EXPERIMENT EXPERIMENTERS

8 11:00 arm. 5 Nike-Cajun Meteorology-ozone, Goddard Space Flight

water vapor Center

9 12:45 p.m. 2A ARCAS 6 MeteorologY Langley Research

Center/Environemntal

Science Services

Adm'inistratio6

10 12:59 p.m. 5 Nike-Apache Meteorology-Pitot Goddard Space Flight

tube Center/University of'

'Michigan

11 1:00 p.m. '4 Nike-Tomahawk Ionospheric physics- Goddard Space 'Flight

thermosphere probe Center

12 1:26 p.m. 5 Nike-Apache Meteorology-pitot Godd'ard Space Flight

g tube 'Center/Universityf of

°-Michigan

CD

N13:27 p.m. ike-Tomahawk Ionospheric physics- Goddard Space Flight

thermosphere probe Center

14 1:35 pam. 1 Aerobee 170 Solar. physics-solar Naval Research

flash spectrum Laboratory

15 1:36 p.m. 1 Aerobee .150 Solar physics-solar Harvard College Ob-

flash spectrum servatoriy/Culhm Lab.,

London/Imperial Col-

lege, London/York

TUniversity, Canada

16 1:36 p.m. 3 Nike-Apache Ionosphericphysics- -GCA Corp./.Lockheed

solar X-rays. Missiles & 'Space Co.

ft.

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NC - LAUNCH TIME :LAUNCil AREA VEHICLE EXPERIMENT EXPERIMENTERS

17 1:37:10 p.m. 2 Nike-Apache Iono'spheric physics- University of Illinois

radio propagation and

electron- measurements-

18 ':37:25 p.m. 4 Nike-;Tom6ahawk Mete6rology-air glow Goddard Space Flight

'Centertj'lniversity of

Maryland

19 1:37:30 p.m., 3 Nike-Iroquois Ionospheric physics- USAF Cambridge Research-

'.potiVe spectrometer Laboiratory

20 1:38 p.m. 2 Nike-Apache Ionospher~ic-physics- University cf Illinois

radio propagation anid

electron mneasurements,

BU 1:39:30 p.m. 3- Nike-Iroquois Ionospheric physics- USAF Cambridge Research

negative spectrometer Laborator-ies

(NOTE: This laurich is S. back-up to be launbhed only if there, is a failure of Launch No-. 19-. If

0 launch 19 is successful, th, s launch will take pl~dce at 3:10 p.m.., March 7.) F,

21 1:40-:30. p.m. Nike-Cajun -MeteOroiogy-ozone Goddard Space Flight

water vapor Center -

22 1:40:40 p.m. 2 Nike-Apache, Ionospheric physics- University of Illinois

-radio propagation and

electron measurements

23 1:41:.p.m. 5 Nike-Apache Meteorology-pitot Goddard Space Flight

pr~obe Center/Universityof -

Michigan

BU '1:45.10 p-.m 2 Nike-Apache Ionospheric physics- University of Illinois

radio propagation and-

elec'tron measuremenrts

, I



~~~XPERIMENTERSib -

NO.; LAUNCk TIME LAUNCH{ AREA VEHICLE EXPERIMENT EPRMNES-

24 . 1:46 p.m. 3 Nike-Iroqudis, Ionospheric physics- USAF Cambridge R&-search

neutral spectrometer Laboratories

25 1:47:16 p.m. 0 Javelin- Ionospheric' physics- TRW Systems C6rp.

neutral hydrogen'flux

26 1:57 p.m. 2A ARCAS 'Meteorology Langley Research

denter/Envicronmental

'Science Services

Administration

27 2:25 p.m. 2A ARCAS Meteorology Langley ReseaIc1 ,Center/Environmental

Science Services

Administratiorn

28 3:00 p.m. 2A ARCAS Meteorology Langley Research

'Center/Environmental M

Science Services;

'Administration

3:10 pn 3 Nike-Iroquois Ionospheric physics- USAF Cambr-idge Research

negative spectromie'er Laboratories

Sunday., Mardch 8

30 11:00 a.m. 5 Nik6-CaJun Meteorology-,ozone,. Goddard Space Flight

water' apor Center

BU 12:25 p;m. 5 Nike-Apache Mete'oro1ogy-Pitot ~GoddardSpnae Flight

tub' Oeiter/Univeriity of'

'Michigan



NO. LAUNCH- TIME LAUNCH AREA VEHICLE EXPERIMENT EXPERIMENTERS

* 12:29 p.m. 2 IINike.C a-'j~ M e'teorolo0gy-Grefl" .de, Goddard Space Flight

expoeriment Center

31 12:115 n,-m. *2A AR AS Me'teorolbgy Langley Reseaarchdenter/EnviroflmentalScience ServicepsAdininist-.iationl

323:00 P.m. 14 Ni-ke-T~omahawk Meteoi~ology-airgioviGoddard Space Flight

32 Center/Ufliversity-ofMary land

Monday, March 9

1U4:30 a.m. 5 Nike-Cajun Meteorolq -~oe odadSae Flight

Waters vap'or Center

*Launch is not connected with eclipse experiments.



LAUiVCH VEHICLES

ARCAS (Atlantic Research Corporation. Atmospheric Sounding)

Single stage moteorbloical rocket

Topal length: 8 feet

Gross weight (less payload): -68 pounds

Jiopellant: Solid fuel

Nominal Payload Weight: 9 1/2 pounds

Diameter: 4.5 inches.

Thrust: 335 pounds

Burning TJ.me: 29 see.

Peak Altitude (with nominal payload): 205,0'00 fee'

Nominal :1.mpact offshore:- 30 NM

'Manufac.turer: Atlantic Research Corporation

Alexandria, Virginia

Nike-ApacheNike-CajunNike-IroquoisNike-Tomahawk

Two-stage soli.d-propellant vehicles using the Nike

booster as the first stage.

First Stage: Nike (M88)'Booster

Length: 12.4 feetPrincipal Diameter: 16.5\inchesThrust: 42.,500 pounds /Burning Time: 3.5 secon4SWeight: 1,300 pounds J

Manufacturer: Hercules Inc.

Radford Virginia

Second Stage: Apache (TE-M-307) r

Length*: 8.9 feet H/

Principal Diamete 6.5 inches

Thrust: 5,000 undsBurning Time: 6.4 seconds

Weight: 270q/ouncdsPeak altitude (Nike-Apache) with nominal

-payload: 585,000 feetTotal length (Nike-Apache): 28 feetManufacturer: Thiokol Chemical Corporation

Elkton, Maryland

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1970 ECLIPSE SOUNDING ROCKETS

T >

ARCAS NIKE NIKE AEROBEE 150 AEROBEE'170 JAVELINAPACHE TOMAHAWK

NIKE NIKECAJUN IROQUOIS



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Second Stage: Cajun (TE-82-4)

Length:' .8.9 feet

Principal Diameter: 6.5 inches

Thrust: 8,500 pounds

Burning Time: 3.3 seconds

Weight: 340 poundsPeak Altitude (Ni1ke-Cajun) with nominal

payload: 250,000 feet

Total Length: 26 feet (Niike-Cajun)

Manufacturer: Thiokol Chemical Corporation-

Elktonj Maryland

Second Stage: Iroquois (TE-M-388)

Length:~ 104.4 inches




Weight: 433 poundsPeak Altitude (Nike-Iroquois) with nominal

payload: 39,0,000 feet

Total Length (Nike-Iroquois): 31 feet

Manufacturer: Thiokol Chemical Corporation

Elkton, Maryland

Second Stage: Tomahawk (TE-M-416)

Length: 142 inches




Weight: 672 pounds

Peak Altitude (Nike-Tomahawk) with nominalpayload: 875,000 feet

Total Length (Nike-Tomahawk): 32.5 feet

Manufacturer: Thiokol Chemical Corporation

Elkton, Maryland

Javelin

Four-stage solid-propellant vehicle

Total length with nominal payload: Approx. 49 feet

Gross weight (less payload): Approx. 7,500 pounds

Net payload weJght:

Minimum - 40 pounds

Nominal - 125 pounds

Maximum - 175 pounds

Peak Altitude: 494 statute miles with nominal payload

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First Stage: Honest John (M-6) Booster

Diameter: 22.9 inches

Length: 16 feet

Weight: 4,300 pounds

Thrust: 82,000 poundsBurning Time: 5 seconds

Manufacturer: Hercules,. Inc.

Radford, Virginia

Second and Third Stage: Nike (M-88) Booster

Length: 12.4 feet

PrIlncipal Diameter: 16.5 inches

Thriust.: 42,500 pounds



Mantifacturer: Hercules, Inc.

iiadford, Virginia.

Fourth Stage: Altair (X-248-A6)Diameter: 19 inches

Length: 6 feet (plus payload, 2.4 feet)


Burning Time: 42 seconds

Manufacturer: Nava" Ordnance Station

Tndian Head, Maryland

Aerobee 150 and 170

Two stage vehicles

Solid propellantbooster first stage

Liquid propellant sustainer second stage

Aerobee 150

First Stage: Aerobee BoosterIX 103C

Length: 6.5 feet

Diameter: 12.75 inches



Weight: 600 pounds

Manufacturer: Aerojet General Corp.

El Monte, California

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Second Stage: Leng 4th: 16 feet

Diameter: 15 inches



Weight (with liquidfuel): 1,550 pounds

Payload weight:

Nominal - 200 pounds

Eclipse payload - 295 pounds

Maximum - 350 -pounds

Total length: Approx. 30 feet

Peak Altitude (nominal payload): 120 miles



Aerobee 170

First-Stage: Nike (M-88)

Length: 12.5 feetPrincipal Diame'ter: 16.5 inches


Burning Time: 3-.'5 seconds


Manufacturer: Hercules, Inc.

Radford', Virginia

Second-Stage: Length: 16 'feet

Diameter: 15 inches

thrust,: 4,100 pounds


Weight (with liquid fuel): 1,550 pounds

Peak altitude (nominal payload): 155 moles



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SCIENTIFIC EXPERIMENTS

Sounding rocket experiments -!ill be flown from Wallopsto make i.nvestigations in three scientific disciplines --

meteorology, solar physics and ionospheric physics.

The following description of the experiments,is keyed to,the launch numbers in the chart , pages 9 thru 13.

Meteorology

Eighteen sounding rockets will be launched from Wallops-carrying meteorology payloads. Primary purpose of these ex-

,periments is to study the response of the Earth's atmosphereto the interruption of sunlight occasioned by the eclipse.

Solar energy has an effect on the meteorological para-

meters (wind., temperature, density, and pressure) of the upperatmosphere which is not uniform at all altitudes.

Since no single rocket experiment can obtain data overthe entire region from 18 1/2 miles up to 62 miles, variousexperiments on five different kinds of rockets with varyingcapabilitites will be launched throughout the day.of theeclipse with several rockets also scheduled for firing on theday before and the day after the eclipse to obtain data onatmospheric condi.tions at the same time of day in the absenceo3 an eclipse.

Temperature and Wind Measurements

Launches No. 2,,5, 7, 9, 26, 27, 28, 31

Eight Arcas rockets will be launched before, during andafter the eclipse to measure the temperature and wind patternsin the middle atmosphere, from 18 1/2 miles to 37 miles. Asecond purpose is to provide data in support-of other eclipseexperiments such as ionization, electron density and ozonemeasurements.

A 1966 eclipse experiment at-a temporary launch site inthe Andes Mountains of Argt..fina showed unexpectedly largetemperature variations in the middle atmosphere region but

some of that data is open to qtestion because of the difficultnature of the operation at the remote launch site and becauseall possible errors were not corrected.

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ECL IPSE OF THE: SUN

THE CORONAL

tss -\

Mob'6ns Orbit

0o -S'

MO S

........



The 1970 launches will repeat th-e experiment using afully equippezd launch site incorporating the latest measure-ment techniques and corrections for errors due to radiation,conduction and aerodynamic heating on the.basis of theoreti-cal studies.

The Arcas rockets will be launched, at precisely spaced.intervals from a launch area about 500 feet north of LaunchArea 2. At coast apogee of about 205,000 feet, a small pay-load called an Arcasonrde is-eJected on a metalized disk-gap-band parachute which is highly reflective for radar tracking.The parachute slowly drifts through the atmosphere while radartracking obtains an'accuiate Wind profile and the payloadtransmits other meteorological telemetry to ground stations.

Principal investigator is Robert M. Henry of NASA-'sLangley Research Center with-Roderick Quiroz of the Environ-mental Science Services Administration (ESSA) National.Meteorological-Center.as co-investigat6r.

Ozone Measurements in Upper Atmosphere

Launches No. 1, 8, 21, 30

One of the important scientific objectives of the eclipsesounding rocket effort from Wallops will be to obtain thefirst high resolution ozone measurements in the upper atmos-phere during an eclipse.

Ozone is found in a region from about 12 miles to about40 m:Lles above the Earth in what is called the mesosphere andthe stratosphere. Although it exists in comparatively smallamounts, ozone -quite literally sustains life on Earth as it

presently exists by absorbing potentially hairmful solar ultra-violet radiation.

Ozone also plays a key role in warming the atmospherebecause heat is generated when-it is decomposed into oxygen.

Understanding the complex chemical process of how ozoneis fornied, how it heats up and how this energy is transferred

in tho atmosphere is a major question facing Meteorologistsin their study of the Sun's interaction with the atmosphere.

Four Nike-Cajun sounding rockets, to be fired fromT~aunch

Area 4, will be used to make measurements of ozone be-'forc and during the eclipse in the hope of finding some ofthe answers to these questions. If there is a failure ofany of these flights, one additional rocket and payload isready to launch as backup.

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The rockets will each carry unique 47-pound ozone-sonde

payloads to altitudes of about 40 miles above the Earth. After

burnout, the sondes will be jettisoned. A parachute will be

deployed to slowly lower the.sensing instrument through the

ozone regions of the mesospher.e and the stratosphere.

Ozone detectors consisting of -a hemiluminescent material

will make continuous readings during descent.. The d&ta willbe telemetered to.ground stations Where it will be recorded

for later analysis.' The payloads will not be-recovered.

The four launchings Xin* the series 'are scheduled at a time

just before.suiirise, about two hours before' the eclipse, during

the period of totality and after. Thus, comparatiVe measure-

ments of nighttime, daytime and -eclipse ozone will be obtained..

Project scientist for the ozone-sonde flight is Ernes't

Hilsenrath of the Godderd Space Flight Center, who also was

responsible for development of the device. The -first -ozone,-

sonde- flightwas.made in September 1968 from Wallops Island.

Uoper Atmosphere Weather Measurements,

Launches No., 3, 10,' 2-,, 23 .

The solar eclipse offers atmospheric scientists. a-rare

opportunity to study the effect on the upper atmosphere of

the abrupt and brief cessation of sunlight which 6ccurs during

an eclipse. Of special interest are changes that occur in

temperature,, pressure and.density in the -c6mplex atmospheric

envelope surrounding the Earth...,

To -find answers t~o these-questions a series of four

Nike-Apache rockets., from Launch-Area 5, will be launched to-

altitudes up to 75 miles under a -program J~ointly sponsor-ed by

the University, of Michigan. nd the Goddard Space Flight Center.-

The device to be flown is a relatively simple pitot tube

not unlike those carried-by modern-day aircraft. This device-,

proven in several years of space flight, provides a reliable

profile of the structure of the' upper atmosphere.

The flight plan calls for four launches, one 24 hours

before -the eclipse-, one when the Sunis obscured about 40

percent, one at 80 percent occultation, and one at totality.

There is one backup rocket and payload. These-flights.will

help -scientists determine normal weather conditions for the

time of year above the launch site and eclipse effects.

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-21-

Scientists conducting the effort are Jack florvath of

the Univeirsity-of Michigan, and Wendell Smith and John Theon

of the GoddardSpace Flight. Center.

Dayglow Obser-vations.

Lauriches No. 18 .32

As energy ;from the Sun enters the upper atmosphere anumber of'-chainges occur, one of which results in the not yet

fully understood phenomenon called airglow.

Airglow is easily observed during nighttime conditions

when it appears as a. ery faint lightness in the sky. Detailed

studies of' its charaic:teristi.cs show-that the glow exhibits

cyclic, seasonal, and often hourly -variations'.

Observing ailrglow during the daytime-(iwhen-it is Lalled

dayglow:). in, the far-u ltraviolet regiopn of the spectrum is

-difficult because of 'the intensity6of Sun light'. Moreobver,

'all of the ultraviolet radiationis absorbed -in he upper at-

-mosphere which means measurements must be~carried out- in space

'itsel'f.-

The solar eclipse offers a unique opportunity tvo study

4ayglow by flying a sounding rocket payload into- -he dayglow

regioni and observing both in the area of eclipse darkness and-

the are'a of sunlight. Of particular scientific interest are

measurements of the abrupt change from sunlight to darkness

during totality at which time rapid changes occur In the com-

poosition of the, ayglow.

To accomplish this objective. the Goddard S-ace Flight

Center has developed a 835-pound payload carryipg- ltravioletphotometers, electron detectors, and spectrometers to be flown

to an altitude of 170 miles by a Nike-Tomahawk rocket from

Launch Area 4 during the period of totality. The payload sen-

sors are mounted in'such a manner that will permit forward and

side viewing during the flight. A second flight will be con-

ducted 24Lr hours after- the eclipse in order to obtain data on

the "normal" dayglow conditions above the launch site. The

data obtained are expected to provide some of the answers to

how dayglow is formed.

Protect scientist for the dayglow flights is Dr. Donald

F. Heath of the Goddard Space Flight Center. lie will be as-

sisted by Dr. Eugene Maier also of Goddard and Dr. Davi'd

Mathews -of the University of Maryland.





-23-

Measurements will also be made of the electric field

and electron density between 55 and 62 miles and of the photo-

electron flux and energy distribution in the E-region. It is

believed that ohotoelectrons may stream in from sunlight por-

tions of the ionosphere, and this instrumentation is designed

to *search for such effects..

Investigators are Dr. 'C. . Accardo, GCA Corp., Bedford,

Mass.; Dr. Nelson C. Maynard, Goddard Space Flight Center; andDr..t 3. W. Sharpe, Lockheed 'Missi'les and Space Co., Palo Alto,

Ca ' -

Rad-o Propagation and Electron Measurements

Launches No. 6, 17, 20, 22

This investigation to be flown on four Ni.ke-Apaches from

Launch Area 2, is designed to measure electron -concedntra.tons,

elec-ron temperatures and electron collision frequencies in

the lower ionosphere during the-eclipse. One rocket will be

launched about three hours before the eclipse, and the other

three during and shortly follow'ing totality. Also to-be ob-served are the density profiles of molecular oxygen and ozone.

Inbtrumentation includes a DC/Langrnuir probe for electron

density and temperaturej a two-f.:equency ('2225 and 3385 kilo--

Hertz) radio propagation-experiment for electron density and

collision frequency,, and solar radiation detectors for X-rays

(44 -oo 60 Angstroms<) and ultraviolet (Lyman alpha and' 2600

Ang~ot Dirs) to observe.molecular oxygen and ozone.

These mecsurements will be correlated with the mass

-pectrometero to he flown by Air Force Cambridge Laborato'r?.es.

Investigators are Drs. Sidney Bbwhill and Eugene Mechtlyof the University or 'Illinois at Urbana and L. G.. Smith of QCA

Cc) p , Bedford, Mass. There is one backup rocket and payload.

'Mass Spec-tr'ometer

Launches No. 9. 924,

Three Nike-Iroquois rockets, nicknamed Niros, will be

fived fror Launch Area 3 to measure the change in neutral

and chiarged particle'concentrations in the D and E regions

01 al: ionosphere between 37 and 87 miles altitude.

Soecifically, the instruments are designed to measure

sirflrlta.zously, and at totality, positive ions, negative ions,

neLt-al constituents, electron concentration, electron tem-

'e 'Vuve, and total positive ion concentration.

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'hese measurements will be compared with others such as

those of solex ionizing radiation. Of special interest will

be a determ~iation of the relative roles of electron attach-

ment and recombination in the absence of sunlight.

One rocket will carry a positive ion, one a-negative ion,

and one a neutral mass spectrometer. Cylindrical Langmuir

probes will be included in the two ion composition payloads.to study the energy distributions of charged particles.

Tnvestigators are Dr. Rocco S. Narcisi, Dr. G. R. Philbrick

and-J. C. Ulwick of the Air Force Cambridge Research Labora-

tor~ies, Hanscom Field, Bedford, Mass.

(High-Altitude Atmospheric Measurements

Launches No. Il, 13

Tw.o Nike-Tomahawk launchings carrying thermosphere probes

will-be flown in.conjunction with the lower altitude pitot

tube meteorological investigationsand to-make ionospheric

studies. These flights are jointly conducted by the Univer-

sity of Michigan and the Goddard Space Flight Center.

The 80-pound probes, ejected after rocket burn-out, are

designed to measure temperature, pressure and density and, in

addition, electron-and ion data at altitudes ranging frz)m 75

to 200 miles above-the'Earth. In these upper reaches the

changing chemistry of the atmosphere is the object of the

research.

The two launchings from Launch.Area 4, are scheduled

during the time of 40 percent and 80 percent darkness. Thus,

comparative analysis of data from the two pitot tube flightsscheduled about the same time will be possible.

Investigators include N. W. Spencer and Larry H. Brace

of the Goddard Space Fl-i.ght Center, G. H. Carignan or the

University of Michigan and Dr. J. C. G. '.!alker of Yale

University.

Energetic Hydrogen Atoms Associated With btye Solar Wind

Launch No. 25

A Javelin, the Largest rocket in the Wallops seri-s, will

be fired From Launch Area 0 carrying an instrumentwhich repre-

sents the first attempt to detect directly a theorized comn-

ponent of the solar wind. The payload will. be in the Moon's

shadow for some 67 seconds at an apogee of 500 miles.

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Some indirect measurements have suggested the existence

of energeti'2 hydrogen atoms associated with the solar wind.

These are believed to arise from charge-exchange of the solar

wind particles with neutral atoms in the interplanetary medium

and possibly, but very urn'ikely, according to the investigators,

as a result of the direct emission of energetic particle.- by

the Sunitself. It is theorized that these may increase greatly

during periods of solar activity.

The neutral atoms will not be deflected around the Earth

in the bow shock, but will penetrate to altitudes as low as

370 miles without significant attenuation. This will be the

first;atteiiwpt to detect directly these theorized neutral atoiis

in the solar wind.

The Javelin will carry two hydrogen energy spectrometers,

one energy independent total hydrogen detector, one Sun sensor

and an aspect magnetometer.

The instrument apertures arearranged so that,.. They will

view the eclip'sed Sun for about Jn percebt of each Sito cycle.

Investigators are William Bernstein,, Dr. Robert L. Wax,

and Dr. George T. Inouye of Space Sciences Laboratory, TRW

Systems Group, Redondo Beach, Calif.

Solar Physicz

Two sounding rockets will be launched from Wallops

carrying solar physics experiments. These take advantage of

the remporary blocking' of the solar disk bi y the Mcon to studythe radiant energy emitted from the Sun's atmosphere and to

study the disturbances that occlur near the Sun's surface and -

their effect on the Earth.

-Particular emphasis will be given to observations of' the

flash spectrum. This radiation originates in a region just

above the visible disk of the Sun, the lower chromosphere.

Ordinarily it is too dim to be seen because of the relativeiy

very bright light of the disk. During the short time tIh't tiff

Moon blocks the light from the disk, the lower chromosphere

becormes visible.

This region As little understood: its temperature is less

than that of the disk --- about 10,000 degrees F. -- while above

this region in the corona, the temperature goes up to about

2,000,000 degrees F. The energy that heats the Sun's corona

passes.through the chromosphere and an understanding of this

is very significant to an understanding of how energy escapes

from tle Sun.

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Regions of the Sun's atmosphere not visible because of

the dimness of its light compared to that of the disk are the

K- and F- coronas. The K-corona can be seen: it is white

light emitted by the disk and scattered by-electrons in the

corona as dim white light (and near ultraviolet and near infra-

red). Observation of this scattered light gives information

on electron densities and temperatures in the corona.

Farther out is the F-corona which can also be seen: White

and infrared light from the disk is scattered by dust particles

farther cut from the Sun where the temperature *is ow enough

that these particles are not vaporized. Observation of this

light, called zodiacal light, gives information on dust in

interplanetary space.

International Solar Flash Spectrum Experiment

Launch No. 15

The experiment,the only international one in the Wallops

series, will photograph the flash spectra or light from the

chromosphere between the corona and photosphere or solar disk

which is too weak to be studied when the Sun is not obscured.

Its purpose is tc further ur.derstand the mechanisms of energy

t;ransfer and heat balance in the region of the chromosphere

and corona some 180 to 12,000 miles above the limb of the Sun.

The flash spectrum will be photographed with two Wadsworth

spectrographs covering the range from 977 to 3,000 Angstroms,

imaging the crescent of the San on the film with wavelength

resolution of one Angstrom. The spectrographs will use no

entrance slit with the Moon occulting the Sun acting as the

entrance slit. Each camera cassette will hold about 25 filmstrips sensitive to exposure times ranging from two-tenths of'

a second to 10 seconds.

The experiment will be launched by ail Aerol-e 150 rocket

and the photographic film must be recovered.

Investigators are Professor Leo Goldberg of Harvard

College Observatory; Professor W. R. S. Garton of Imperial

College, England; Professor R. W. Nichols of tite Center for

Research in Experimental Space Sciences, York University,

Canada; and Dr. R. Wilson of the Astrophysics Research Unit,

Culhari Laboratory, England.

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Naval Research Laboratory Solar Flash Spectrum Experiment

Launch No. 141

This experiment will study the solar flash spectrum

originating in the chromosphere by observing in ultraviolet

light between 1400 and 2000 Angstroms. Thi's region can be

investigated by measuring the intensities of a variety ofemission lines which have different stages of ionization and

therefore can be seen best in the ultraviolet. The eclipse

which uses the Moon occulting the Sun as part of the imaging

system offers a unique chance for high angular resolution

measurements.

The temperature and iron abundance of the inner corona

can be studied only by measuring lines of very highly iohized

elements. The absence of stray light from the solar disk dur-

ing the eclipse makes it possible to obtaifn much purer spectro-

heliograms of-the corona..

in addition, the transition region far out in she coronaproduces the zodiacal light and is one of tie least known

spheres around tie Sun. By measuring the irntensity and polar-

ization in different color bands, the experimenters will try

to determine electron and dust particle density out to ±,more

-than 2,000,000 miles from the Sun.

Five instruments will be flown on an Aerobee 170 rocket

to be fired from Launch Area 1. All will be fine-pointed at

the Sun by means of' a special eclipse pointing system developed

by the Naval Research Laboratory. The instruments are:

- Wadsworthsoectroheliograph covering 150 to 437

Angs'roms to study the flash spectrum;

Wadsworth spectroheliograph covering 727 to 1060

Angstroms to study the flash spectrum and Lyman radiation;

-Modified Wadsworth spectroheliograph to study Tyman

alpha radiation in thle flash spectrum;

- Wadsworth spectroheliograph covering '.350 tr 1900

Angstroms to study the flash spectrum and far limb spectra;

- Multichannel Wadsworth configuration ,canring spectro-

mester covering '300 to 2000 Angstroms to obtair onecomplete

s'ectrum in hall a second.

Investigators are J. D. Purcell, Dr. G. E. Brueckner

and Dr. R. Tousey of the E. 0. Hulbert Center fcr 'Space Re-

.;earch, Naval Research Laboratory.

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WALLOPS RANGE OPERATIONS

An elaborate complex of tracking and communications

equipment, for sounding rocket research at Wallops Station,

will provide the precise tracking and data acquisition

required for the 1970 solar eclipse project. Never have so

many types- of data-seeking rockets been launched within-such

a short time as for thiseclipse. This considerably increases

the normal problems involved in launching, tracking and data

acquisition.

The.size of the project requires- the full time use of

most of the staff and facilities at Wallops Station. In

several areas addit.ional personnel-and equipment have been

provided.

Fourteen of the 32 rockets involved in this project-will

be sent aloft within some 20 minutes, seven within less than

two -mnutes.,. .t the height of the eclipse. Fourteen additional

rocket launchers have been-ins'tal-ed on Wallops Island, making

a total o'f twenty-four launchers to accomplish the March 7"barrage."

These rockets all require accurate position and velocity

data which is provided by ground:-based radar systems. -To

assist the radar systems in distinguishing betWeen- the many

targets, most rockets will carry a small transponder which.

has an identifying code.

Wallops Staticn., supported by NASA's Office of Tracking

and Data Acq'ulsition, has installed six mobile S-band radars

6o supplement the seven permanently installed radars. These

mobile units were surplus equipment obtained from the Manned

Space Network and the Air Force. A special synchronizationsystem is being developed to minimize the interference between'

radar systems.

Most of the scientific data is telemetered back to

Wallops. Again because of the large number of rockets,

additional equipment has been installed. Some deactivated

systems have been activated and the new S-Band telemetry

antennas have been modified to cover the VHF telemetry band.

Most of the telemetry will be received by the Wallops

mul]tiple. telemetry station, but this will be augmented by

two telemetry vans on the Station and two mobile units from

the Goddard Space Flight Certer. In addition, the Wallops

telemetry shin, USNS Range Recoverer, will be on station off

the Virginia Coast. The ship also will serve as a backup in

payload recovery operations.

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Two rocket flight experiments (the Aerobee 150 and 170)

will be dependent upon payload recovery from the ocean to

obtain the scientific data recorded on photographic film

during flight. Extensive primary and contingency recovery

plans and techniques have been devised to insure the full

realization of scientific data potential from the two re-

coverable payloads which will splashdown in the Atlantic

Ocean.

The recovery plans and techniques developed at Wallops

Station will employ specialized equipment and the combined

teamwork of various- groups of operating personnel. Recovery

-forces include four fixed-wing search aircraft, three surface

recovery vessels, three recovery helicopters, UDT diving

teams, and radar,, communication, telemetry, photographic,

-and ground support equipment teams. Assistance and recovery

units have been obtained from the United States Coast Guard,

Navy, NASA and private contracting sources. Planning and

direction of the recovery operations is the responsibility of

Wallops Station.

In addition to the main Range Control Center (RCC),

several subordinate control centers have been established for

pad clearance, payload checkout, telemetry checkout and radar

control for all rocket launchings in their individual areas.

These three "satellite" control centers are located near

rLaunch Areas 1, 2, 3, and 5. The main RCC will serve

as a coordinating and monitoring point for the "satellite"

centers and as the Control Center for recovery operations.

During totality when a few launchings will take place

at 10-second intervals, these centers will essentially be

on tneir own. The Project Manager will be in the main RCClocated on the Wallops Main Base, approximately five miles

northwest of the Island launch complex. The Island Test

Director3 will be located in the subordinate Control Center

blockhouses. Communication between the many engineers,

technicians, and-scientists is accomplished by a 15-channel

operational intercom system. Communication with the recovery

ships and aircraft is by HF and VHF radio.

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WHITE SANDS MISSILE RANGE SOUNDING ROCKETS

Two sounding rockets sponsored by NASA will be launched

from White Sands in support of the Wallops sounding rocket

launches.

Naval. Research Laboratory Solar Experiment

An Aerobee 150 rocket will be launched from White Sands

just before oir just after the eclipse, the most desirable

launch time being 7:00 a.m. EST. During the total eclipse

on the East Coast, the Sun will be partially eclipsed at

White Sands but the payload pointing control cannot operate

properly without full sunlight.

The Aerobee,, with an experiment package containing five

experimentsa, will be launched to an altitude of 113 miles and.

is scheduled tobe recovered., All instruments- in the package

will be pointed at the Sun by a University of Colorado biaxi~al

solar pointing control.

The payload carries:-

- Two photographic coronagraphs extended on a 30-inch

spar which will be stowed inside the instrument package during

launch phase. The coronagraphs will artificially eclipse the

Sun with a circular occulting disk. Some 50 exposures will

be made, each of which will photograph the visible corona from

1.3 to 3.9 million miles from the Sun with exposure taimes from

two to six seconds, The Moon w.ill be in the field of view

providing a unique calibration point.

Three other experiments are closely related:

- A photographic extreme ultraviolet spectroheliograph

which consists of a concave grating and photographic film. A

spectrum of solar disk images in the range from 170 to 650

Angstroms will be photographed.

- A photographic extreme ultraviolet heliograph which

consists of a concave mirror, photographic film and a thin

aluminum filter which allows the solar disk to be photographed

in the 170 to 650 Angstrom bald.

- An ion chamber which measures solar flux in the strongLyman alpha emission by a suitable combination of window

material and gas fill.

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Rapid recovery of the-film from the coronagraph, spectro-

, heliograph and heliograph experiments is required.

Project scientist is Martin J. Koomenaof the U. S. Naval0

Research Laboratory..

tAS&E Ec-lipse Photography

'Another eitobee 150 rocket will -be launched from 'White

Safids as close to the tim& of totality at Wallops as possible

to gather data for Comparison with the Wallops data.. The- peak

altitude should be about 105 miles.

This American Science-dnd Engineering Inc. experiment is

-designed to ob~tain high-resolution pictures of the-time develop-

ment of the -eclipse in the X-ray region of the spectrum. The

de-occultationf-of' hee-corona by the 'Moon will be' seen in X-rays.

In flight, a ffine-inch diameter X-ray telescope is used

to focus the solar ,image onto a 35-mm motion picture camel-a

.which runs at, one frame per second. Just in front of the

camera, a wheel_- ith.five filters steps one posi-tion between

each- frame..'

The--various filters on the wheel transmit data in

different passbands, :giving spectral information and pirovid-

ing some latitude in exposu3re'time. One filter passes visible

light to the camera, providing a reference image for correlating

the X-ray images-with visible observations from the ground.

During the -picture taking period, a photbmultipi-ie-r/

scintillator assembly mounted at the front ofthe experiment

monitors X-ray emissions. Its purpose is to provide an accurate

measurement of changes in several spectral regions during

the period of the eclipse.

Because this is-a photographic experiment, the payldad

will be parachuted to Earth, and rapid recovery is required.

The scientific experimenter is T. F. Zehnpfennig of

American Science and Engineering, Inc.

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ATS-3; Pctures During Eclipse

A spin scan camera on Applications Technology Satellite-3

will be6taking.pictures of the nort1hern hemisphere of the Earth

at~the time of the ec1ipsq.It is.expected that the shadow.

of the-*-e,clinse oi, the. Earth will -be seen in the photographs as

a shadow on the white cloud'cover. If the shadow is over a

dark land .masq it is. not. eipected.-to be seen.

Sinc& te umbra.(the region.,of -deep shadow-) -moves about

six milesper second and the ca eta scan period is six.-tenths

of a secoqndj, some. distortion of the. shape of the ecli-pse must

be expected.^

Although the camera can photfgraph the whole Earth, the-

.mode o-f camera opeirati-on--will be changed to scan only the

norther'n hemisphere to incr-ea'e the number of6-ecdise pi-ctures-.

Data wlllbe, received in real time from ATS-3. Since it takes12. o 15 minutes' for each -picture of the northern hemisphere,.

4as many.- as '8 to-'i2 ,pictUre-s cou-ld be taken of'the-eclipse

shadow..

The data-willbe- eceived- at NAS'A's 'Rosman, N.C., station

and, transmitted to tie Goddard' Spade Flight, Certer where the

pIctures will be sc ann!etd and phot`ograghed..

,SO's 5 and 6 Observations

,Two spacecri',itt specifically designed, o study the Sun from

Ea~ihth orbit, OrbitingSolar Observatories 5 and 6, will each

make two- passes thr.ough-_egions' of'partial eclipse -on March 7.

The 0O0 spacecraft, which isc spin-stabilized, -also has

several instrurents mounted in a "sail" portion- of the space-

craft which is cohtinuously pointed at the Sun. Data- from these

instruments will be of specia:l infterest and all OSO eclipse data

will be s'ent to the investigators, as- quickly as possi1ble.

Both OSO_'s wi11 be in .position to see the eclipse in about

-o '80to0.-per c enf~toa.ity.'- S3,- 'will1read out its data t'o the

N'ASA.racking stta-i-. at Santiago., Ch'ile.- OSO 6 will read out

t'to.the Fort e F-la.., tracking statifon which wil"l send it in

real time to the `'cddard Center,

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At Goddard, the data from one OSO. 6 experiment,,, the HarvardCollege Observatory -ultraviolet spectrometer arnd 'spectro-

heliometer can be displayed.in real time on a color cathode raytube to be photographed. It i- s anticipated that-the eclipse

will be observed in these data.

Canadian Satellite Studies

Three satellites launched by NASA -in the joint U.S./

Canadian International Satellites for Ionosphericd"Studies (ISIS),

Program will be -used to-study the e~ffect of the eclipse on, thetopside ionosphere. All are in high inclination orbits and at

various altitudes: Alouette I in a circular 620.-mile -orbit

Alouette T, in.an elliptical 310-by-1860 -mile orbit -and I<SIS-I

in a 353-0by,.-2182-mile orbi't.

*For this eclipse, Alouehtte, II, and ISIS-I will be in-the bestposition, crossing the eclipse regi2oh 52 and 27 minutes after-

totali ty.

All these satellites are capapble of taking topside. iono-

grams at i-itervals -of 20 to 30 seconds. These are "depth"soundings of the ionosphere from ablovbe, similar to the soundings,

of the qaea bottom made by sh-iPs. It is planned to sample the

eclipse region -sevgeral days before and after thef vent to -obtain

control i-nforriation, During the- eclipse- a continuous. run of'records will be taken frtofn the equator through the eclipse

r'egion and far to the north. From these records, the heightdistribution of electrons, at 90-mile intervals along tle- orbit

will -be calculated and compared -with similar data from thecontrol days.

Investigator will be Dr. G-. L. Nelms ofrthe -Department ofCommunications, Communications Research--Centtre, Canada. Thedata will be shared by an ISIS wbrking group composed ofparticipants from several nations.

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'GROUND-OBSERVATIONS

-Observers from three univer~sities and. three NASA field,.centers

will study the eclipse from three locations under NASA sponsor-

'sh''ip..

White-Ligh-t Photography of- Corona

A'University -of Mich-igan team- ill take photographs of

the,, - lar corona concentrating -on the K-corona or 61e~ctron

pro. 'Led,'c~orona in an 'attempt to ' relate doronal.structures to

featur'es, of, the chromosphere.b The observations, will also

obtainhdata -on .the di-stributi-on,of electron densities within

the c&ordn&a at the itime of' &clipse>.

The obse'Vat'ions, wili 'be made. at a sma'-l -NASA site .on

a:bsack. bay of a national wildlife refuge near Sahdbridg, 1Virginia, south of Virginia Beach.'

Using a portable coelih~stat',.wh'i'cn isa pointi-ngdevice

with a 1'4'-inch diameter .mirror, pictures will be takenr with a

25-foot focal -ength -camera. Corona-l radiation between,4,000

;and 5. 00 Angstroms will 'be,,captu. ed on 8 by 10 inch plates.

Investigators from the, epartmenti of Astronomy and the

McMath-Hulbert Observatory of the University -of'Mich'Igan 'at

-Anri Arbor are Drs. R.G. Teske and O0.C. Moh-l6r,.,"Mrs. Ann'

Hutchinsonj John Iwanski and, Tevfi-k Soyumer.

,Flash Spectra of the Chromosphere

A Langley Research Center expeqrimei-ter, also at the

Sar db id e site will photograph 'the solar flash sp6ctrumrf,

.i'ght from the chromosphere, between the corona and the disk

too'. weak to be seen when the Sun is not obscured,. It can be

photographed just before the.Sun becomes totally-eclipsed.

The objective is to obtain the solar flash spectrum in

wavelengths f'rom 3,100 to 9,000 Angstroms to compare with

-previous flash spectra and other 1970 eclipse- observatiorn5.

It is hoped to obtain very faint lines over the full spectral

range.

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''o enhance the observations, the Langley Center hasrequested merchants in.nearby Hampton and Newport News,

Va. to turn out the lights associated with theirbusinesses, particularly large outdoor advertising displaysduring the period of the eclipse.

The Colorado instrument will use an optical--assemb~lyfor two Wollaston prisms on Lan-ley's 9 1/2-inch Cassegraintele- ope. The purpose is to investigate the difference betweenthe Solon of tangentially and radially. polarized radiati6nfrom the solar K-corona. The two polarized components will beseparated by the Wollaston prisms placednear the image in thetelescope to study the color by tworcol~or photographic photo-metry. if the experiment is successful, it should aid-three-dimensional Interpretation of coronal photographs to be takenby observers elsewhere.

The investigator Ant the University of Colorado is Dr.

Donald E. Billings.

Photography of Coronal Structure

This experiment by NASA's Ames Research Center will usea better resolution of the low contrast, intermediate scale-structure of the K-corona or electron corona to study thecoronal structure,

To photograph the full intermediate scale coronal structure,the extreme' brightness oJ. the inner corona must be reduced ina uniform manner before the light reaches the film to avoid overor under exoosure. To accomplish this, a specially shaped

rotating sectorwedge called a radial transmission filter willbe fabricated at Ames and mounted an inch or two in front.of the

prime focus of the telescope.

Ten to twenty exposures at varying exposure times will bemade with a 70mm camera on Plush X pan film with a red gelatinfilter used to reduce the background sky brightness..

TIhe investigators fo r the Ames Research Center are SheldonM. Smith and Milton Henderson and for Lanigley, Leonard M.Weinstein.

Photoelectric Photometry of the Solar Corona

A Langley Research Center experiment will be conductedin the path of totality at Miahuatlan, Mexico. It will useNASA's Satellite Photometric Observatory, a completely mobileand self-supporting facility, originally built for precisiontracking of satellites.

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The Observatory, housed in a 16-ton truck, is a 24-inch

Cassagrainian telescope, a four-axis tracking mount, and a

four-channel, cryogenically cooled phototube detection system

for intensity and dual-beam polarization measurements.

The purpose of the experiment is to determine the intensity

of the coronal radiation to an accuracy of one per cent.

Simultaneous mideband multicolor measurements of the intensity

and polarization of the coronal radiation will be made out to

some 1wo million miles from the Sun in an effort to determine

for the first time the. fine structure of the coronal electroi

density and temperature.

The instrument will make gradually increasing spiral scans

from the center of the lunar disk occulting the Sun out to some

two, million mIles from the Sun.

The scientific investigator is David S. McDougal of theSpace Environment Branch, Langley Research Center.

Multiple Eclipse Studies

A team of NASA Manned Spacecraft Center and University of

Houston scientists will make a variety of observations near

Miahuatlan, Mexico. The main objective deals with the

separation of the F and K coronae, the structure of the corona

and study of interplanetary dust and particles with experiments

that can be carried out only during an eclipse. This will

provide a large amount of ground-based data for use by the

solar experiment on the Ap6llo Telescope Mount.

One experiment will measure the intensity of the corona

in an observation line so that only the K corona will be

recorded. Comparing this with the light of' the combined F

and K coronae will obtain the contribution of the F'corona.

Thus it will be possible to determine the distribution of

interplanetary particles in the vicinity of the Sun.

Another experiment will measure coronal radiation out

to ten degrees from the Sun to gather information on the

scattering properties of interplanetary particles responsi-

ble for the outer I' orona and zodiacal light.

A flash spectrum experiment will record the spectrum of

the chromosphere just before and after totality to gather data

on the temperature distribution within the atmosphere,

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Photographs with exposures of varying lengths will be

taken during totality to detect faint comets predicted to be

found near the Sun.

Photographic and photoelectric techniques will be used to

determine the size, velocity and intensity of the shadow bands.

These are produced just prior to and just after total eclipse

when a small part of the photosphere or solar disk is visible

behind the limbs of the Moon. The light is spread in a

diffractions pattern and moves across the surface of the Earthat a high velocity. Very little is known about the nature of

these bands and they have never been detected photographically

or photoelectrically.

Investigators are Dr. Robert- P. Kovar, Dr. Jack Reid, and

George P. Bonner of the Manned Spacecraft Center; N. K.. Shankarof Lockheed Electronics Co.; and Dr. Natalie S. Kovar of the

University of Houston.

-end-

Documents

1970 Solar Eclipse Press Kit