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

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

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

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

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

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

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

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

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

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

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

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

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

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