Comparison between IBIS Observations and Radiative Transfer Hydrodynamic Simulations of a Solar Flare

Fatima Rubio da Costa1, Lucia Kleint2, Wei Liu3,4, Alberto Sainz Dalda3,4 and Vahe Petrosian3, (1)Stanford University, Department of Physics, Stanford, CA, United States, (2)University of Applied Sciences and Arts Northwestern Switzerland, Windisch, Switzerland, (3)Stanford University, Stanford, CA, United States, (4)Lockheed Martin Solar and Astrophysics Laboratory, Palo Alto, CA, United States
Abstract:
High-resolution spectroscopic observations of solar flares are rare but can provide valuable diagnostics. On September 24, 2011 an M3.0 class flare was observed by the Interferometric BIdimensional Spectropolarimeter (IBIS) in chromospheric Hα and CaII 8542 Å lines and by the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) in X-rays. We fitted the RHESSI spectra at different times with a power-law plus isothermal component. We then used the fitted real-time spectral parameters of nonthermal electrons as the input to the RADYN radiative hydrodynamic code (Carlsson et al, 1992, 1996; Allred et al, 2005) to simulate the low-chromospheric response to collisional heating by energetic electrons. We synthesized both the Hα and CaII 8542 Å lines from the simulation results and compare them with the IBIS observations. We discuss the constraints from this comparison on particle acceleration mechanisms in solar flares.
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