HR: 11:15h
AN: SP52A-04    [Abstracts]
TI: Chromospheric Response to Non-Thermal Electrons During Flares Using RHESSI and SOHO/CDS
AU: * Milligan, R O
EM: r.milligan@qub.ac.uk
AF: Queen's University Belfast, Dept. of Pure and Applied Physics. University Road, Belfast, BT7 1NN United Kingdom
AU: * Milligan, R O
EM: r.milligan@qub.ac.uk
AF: NASA Goddard Space Flight Center, Code 682, Greenbelt, MD 20771 United States
AU: Gallagher, P T
EM: peter.t.gallagher@ucd.ie
AF: NASA Goddard Space Flight Center, Code 682, Greenbelt, MD 20771 United States
AU: Gallagher, P T
EM: peter.t.gallagher@ucd.ie
AF: L-3 Communications GSI, NASA Goddard Space Flight Center, Greenbelt, MD 20771 United States
AU: Gallagher, P T
EM: peter.t.gallagher@ucd.ie
AF: University College Dublin, Dept. of Experimental Physics Belfield, Dublin, Dublin 4 Ireland
AU: Mathioudakis, M
EM: m.mathioudakis@qub.ac.uk
AF: Queen's University Belfast, Dept. of Pure and Applied Physics. University Road, Belfast, BT7 1NN United Kingdom
AU: Keenan, F P
EM: f.keenan@qub.ac.uk
AF: Queen's University Belfast, Dept. of Pure and Applied Physics. University Road, Belfast, BT7 1NN United Kingdom
AB: Many current solar flare models predict a relationship between the amount of energy deposited in the chromospheric and transition region layers of the solar atmosphere by non-thermal electrons, and the velocity at which this superheated material rises. For the first time, we present findings from simultaneous observations of loop footpoints using RHESSI and SOHO/CDS. RHESSI HXR images and spectra are used to determine the flux of non-thermal electrons using the thick-target bremsstrahlung model, while upflow velocities in the Fe XIX emission line are observed using CDS.
DE: 7507 Chromosphere
DE: 7519 Flares
DE: 7546 Transition region
DE: 7549 Ultraviolet emissions
DE: 7554 X rays, gamma rays, and neutrinos
SC: Solar Physics Division - AAS [SP]
MN: 2005 Joint Assembly