June 7, 2015 Kelly E. Korreck Smithsonian Astrophysical Observatory Kelly E. Korreck...

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

– 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

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 (john.m.davis@nasa.gov)– Tetsuya Watanabe (watanabe@uvlab.mtk.nao.ac.

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

– SOT: T. Berger (berger@lmsal.com)– XRT: L. Golub (golub@cfa.harvard.edu)– EIS: J. Mariska (mariska@nrl.navy.mil)

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

June 7, 2015 Kelly E. Korreck Smithsonian Astrophysical Observatory Kelly E. Korreck...

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