HR: 1330h
AN: SP23B-07    [Abstracts]
TI: Reconciling Hydrodynamic Simulations With Yohkoh and RHESSI Observations of Solar Flares
AU: * Warren, H P
EM: hwarren@nrl.navy.mil
AF: Naval Research Laboratory, Code 7673HW, Washington, DC 20375 United States
AB: High spatial resolution TRACE observations provide compelling observational evidence for small-scale filamentation in solar flares. In this poster we present results from time-dependent hydrodynamic simulations that treat a flare as a succession of independently heated filaments. The energy deposited onto each filament and the volume of each filament are derived from the observed GOES soft X-ray fluxes. These numerical simulations are able to reproduce both the evolution of the line intensity and the shape of the line profile for the Yohkoh BCS Ca XIX and S XV lines. Of particular significance is the fact that the simulated line profiles are always dominated by the stationary component, consistent with observations. In this model the strongly blueshifted emission evident during the initial heating of a thread is largely masked by emission from threads that have been heated previously and do not show bulk motions. In addition to comparisons with Yohkoh we will also present detailed comparisons between simulation results and RHESSI flare observations.
DE: 7519 Flares
SC: Solar Physics Division - AAS [SP]
MN: 2005 Joint Assembly