1. XRT Particle Acceleration at Magnetic Reconnection Sites
72.06 Kelly E. Korreck
Harvard-Smithsonian Center for Astrophysics
Cambridge, MA
December 1, 2018
Kelly E. Korreck
Smithsonian Astrophysical Observatory

2. Smithsonian Astrophysical Observatory
Outline
Reconnection and the Sun
Past Observations and Status
XRT and particle acceleration
On disk flare
Future Prospects for Solar Reconnection Studies
December 1, 2018
Kelly E. Korreck
Smithsonian Astrophysical Observatory

3. Solar Missions and Reconnection
Yohkoh
Courtesy of JAXA
Cusp structure at the top of a flare loop discovered by Yohkoh , and hard X-ray sources above a flare loop (the contour lines in white) . These discoveries are regarded evidence for magnetic reconnection.
December 1, 2018
Kelly E. Korreck
Smithsonian Astrophysical Observatory

4. UVCS CME results: Reconnection physics
On several occasions, narrow brightening in Fe XVIII (Te ~ 6 MK) appears in the probable location of a current sheet.
Lin et al. (2005) also saw Lyman alpha “closing down” in the sheet: one can measure reconnection rate (Vin / Vout )
UVCS is built for UV spectroscopy and Visible light polarimetry of the solar corona
Slide Courtesy of Steve Cranmer

5. Science Questions to Address with Hinode Data
The three instruments are designed to provide coordinated observations that will follow the generation, transport and ultimate dissipation of magnetic energy from the photosphere to the corona.
Coronal Heating
Reconnection, particle acceleration,and jets
Flare Energetics
Coronal Mass Ejections
December 1, 2018
Kelly E. Korreck
Smithsonian Astrophysical Observatory

6. XRT Science Goals for Reconnection Studies
Reconnection and Jets
Where and how does reconnection occur? Is it related to slow CMEs?
High time resolution
Large FOV
What are the relations to the local magnetic field?
High spatial resolution
Broad temperature coverage
Coordinated observing with EIS/SOT
December 1, 2018
Kelly E. Korreck
Smithsonian Astrophysical Observatory

7. Length Scales and Temperatures in Reconnection Sites
Scales to consider
Height in the corona
Length of field lines/separation of loop foot points
Differences in peak electron and ion emission
Flare reconnection/acceleration site for electrons were found to be at a height in the corona of ~107 meters from type III radio bursts.
December 1, 2018
Kelly E. Korreck
Smithsonian Astrophysical Observatory

8. Smithsonian Astrophysical Observatory
SXT
&
XRT
December 1, 2018
Kelly E. Korreck
Smithsonian Astrophysical Observatory

9. TRACE & XRT are Complimentary
December 1, 2018
Kelly E. Korreck
Smithsonian Astrophysical Observatory

10. Smithsonian Astrophysical Observatory
December 1, 2018
Kelly E. Korreck
Smithsonian Astrophysical Observatory

11. Smithsonian Astrophysical Observatory
On disk loops
C_poly
Al_med
Al_poly
Size Scale of Loop
Length of Loop
5 x 106 m
Height~107m
The box is ~30 pixels across with is 2x10^7 Meters in “loop height” and 15Mm
Be_med
December 1, 2018
Kelly E. Korreck
Be_thin
Smithsonian Astrophysical Observatory

12. Smithsonian Astrophysical Observatory
Complimentary Data
284 A
TRACE adds information about structure as well as more filters for temperature analysis
December 1, 2018
Kelly E. Korreck
Smithsonian Astrophysical Observatory

13. DEM Temperature Determination
Log T=5.9 * *
Log T=6.5 *
December 1, 2018
Kelly E. Korreck
Smithsonian Astrophysical Observatory

14. Conclusions and Future Work
Height of site agrees with past results.
DEM temperature characterization needs a full set of filter wheel observations to really characterize the sites
Coordinated SOT/XRT/EIS reconnection site observations to get high time cadence and many filter (temperature) observations
Use Rhessi data to understand the characteristics of the electrons in the process
Modeling of these reconnection sites
December 1, 2018
Kelly E. Korreck
Smithsonian Astrophysical Observatory