X-ray Emission from Flaring Loops: Comparison Between RHESSI Observations and Hydrodynamic Simulations

Details X-ray Emission from Flaring Loops: Comparison Between RHESSI Observations and Hydrodynamic Simulations X-ray Emission from Flaring Loops: Comparison Between RHESSI Observations and Hydrodynamic Simulations

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006spd....37.2705l&link_type=abstract

American Astronomical Society, SPD meeting #37, #27.05; Bulletin of the American Astronomical Society, Vol. 38, p.254

Astronomy and Astrophysics

Astronomy

Scientific paper

RHESSI with its high temporal, spatial, and spectral resolution has revealed many interesting results on the X-ray emission from solar flares, some of which can shed light on the processes of energy release, particle acceleration, heating, and evaporation of chromospheric plasmas. During the impulsive phase of a limb flare, Liu et al. (2006) reported hard X-ray (HXR) emission dominated by the legs of the loop, as opposed to the commonly observed loop top (LT) and footpoint (FP) emissions. The HXR emission tends to rise above the FPs and eventually merge into a single LT source, suggestive of a gradual density increase in the loop possibly caused by chromospheric evaporation. During the decay phase of six limb flares, Jiang et al. (2006) found that the thermal LT source is confined in a small region near the top of the loop rather than spreading throughout the whole loop. The total energy of the source decays much slower than expected from the classical Spitzer conductive cooling alone. A quasi-steady loop model that includes significant suppression of thermal conductivity and/or continuous heating of the LT plasma, presumably by plasma wave turbulence, was proposed to account for this observation. A more thorough understanding of these phenomena requires a solution of the time-dependent hydrodynamics of the flaring plasma. We have embarked on combining our particle acceleration and transport code with a one-dimensional hydrodynamics code (Mariska et al. 1989) to simulate the response of the atmosphere to the energy input during the impulsive and decay phases, and investigate the effects of such response on the energy transport, X-ray radiation, and even particle acceleration and plasma heating processes. Current results from this work in progress will be presented. We will also compare the results with RHESSI observations and thus put important constraints on theoretical models.

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