June 7, 2015 Kelly E. Korreck Smithsonian Astrophysical Observatory Kelly E. Korreck Harvard-Smithsonian Center for Astrophysics Cambridge, MA X-ray Observations

April 18, 2023Kelly E. Korreck

Smithsonian Astrophysical Observatory

Kelly E. Korreck

Harvard-Smithsonian Center for Astrophysics

Cambridge, MA

X-ray Observations of Solar Magnetic Reconnection Sites



Outline

• The satellite and the instruments

• What was the state of understanding with Yohkoh

• Science questions to be answered

• First look at Hinode data

• What else we will do with Hinode data

• Other questions/future work



HINODE (Solar-B)

JAXA, NASA, & PPARC– Solar Optical Telescope (SOT)

• Magnetic fields, photosphere, & Chromosphere (LM, NAOJ)

– EUV Imaging Spectrometer (EIS)• Transition Region, Corona (170-210 Å &

250-290 Å) (NRL, MSSL)

– X-ray Telescope (XRT)• Corona, Soft X-rays (6-200 Å)• G-band 4305 Å • SAO & JAXA

Sept 22, 2006

Uchinoura Space Center, Japan



• Wolter-I grazing incidence mirror with co-focal visible light optics

• 2048x2048 back-illuminated CCD 13.5 µm pixel size

FOV 34 x 34 arcmin

Plate scale 1”/pixel



Field of View

• SOT– Broadband Filter Imager

(BFI)

– Narrowband Filter Imager (NFI)

• EIS– 1” & 2” slits

– 40” & 266” wide Slots

• XRT– Full Sun & smaller



Theoretical Temperature response for unit volume emission measure of 1044.0cm-3 for each filter.

Transmission profiles for filters, X-ray reflectivity of mirror, & qE of CCD detector are taken into account.



Filter comparison

Al Poly

Al-Poly



Filter comparison

C Poly

C-Poly



Filter comparison

Be Thin

thin-Be



Filter comparison

Be ThinAl Poly C Poly

11/22/2006 17:53UT



SXT&XRT



SXT&XRT



XRT & SXI



TRACE & XRT are Complimentary

XRT 11/13/06

TRACE 11/13/06



First 90 days

• Coronal Voids

• X-flare

• Jets, Outflows, Downflows

• Coordinated observations with EIS & SOT

• Global Coronal Activity

• Quiet Sun



Loops on the Limb

QuickTime™ and aPNG decompressor

are needed to see this picture.







Determining Temperatures

•Useful for understanding location of flare heating, cooling processes in flares and solar eruptions.

•Method 1 - Filter Ratios

•Method 2 - Differential Emission Measure Analysis



Observations



Filter Ratio Analysis



Filter Ratios

* **



Filter Ratio Analysis



DEM Analysis

•Method developed by M. Weber, E. DeLuca, L. Golub (see L. Golub et al., 2004)

•DEM determined by a least-squares minimization algorithm

•Random error generation for determining DEM errors



DEM Analysis

ambient corona flare loop



DEM Analysis

ambient corona flare loop



Emission Measures inDifferent Temperature Bins

2-3 MK 3-5 MK 5-10 MK



Emission Measures inDifferent Temperature Bins

10-20 MK 20-50 MK 50-100 MK



Where is the Hot Plasma?



Conclusions so far...•Post-flare loops contain multi-

thermal plasma, ambient corona is closer to two-temperature plasma

•Hot plasma is not well determined using this method with only XRT data

•RHESSI data should be useful in constraining high temperature plasma



Stay tuned for more great XRT flare data as solar maximum

approaches...



CMS models



Acknowledgements

• P. Jibben for this wonderful template

• The entire XRT SAO team



Access To Hinode Data

• Chief Coordinators:– John Davis ([email protected])– Tetsuya Watanabe ([email protected].

jp)• Science Schedule Coordinators (in U.S.):

– SOT: T. Berger ([email protected])– XRT: L. Golub ([email protected])– EIS: J. Mariska ([email protected])

• XRT Observing (XOB) Proposals: http://solar.physics.montana.edu/HINODE/XRT

mailto:[email protected]




















Documents

June 7, 2015 Kelly E. Korreck Smithsonian Astrophysical Observatory Kelly E. Korreck Harvard-Smithsonian Center for Astrophysics Cambridge, MA X-ray Observations