On the cooling processes of solar flare loops in the gradual decaying phase---Suppression of conduction and heating by plasma wave turbulence

Details On the cooling processes of solar flare loops in the gradual decaying phase---Suppression of conduction and heating by plasma wave turbulence On the cooling processes of solar flare loops in the gradual decaying phase---Suppression of conduction and heating by plasma wave turbulence

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsp23b..05j&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #SP23B-05

Astronomy and Astrophysics

Astrophysics

7500 Solar Physics, Astrophysics, And Astronomy, 7519 Flares, 7554 X Rays, Gamma Rays, And Neutrinos

Scientific paper

High spectral and spatial resolution observations of RHESSI show that emission in the gradual phase of many solar flares is dominated by a thermal looptop source, which cools down faster than expected from the radiative cooling but much slower than that due to the cooling by classical Spitzer conductivity. This could be due to a continuous energy input at a rate equal to the conduction rate. One would then expect a nearly isothermal loop with an almost uniform emission along the loop and significant energy injections at the foot points. However, the looptop image is resolved along the loop and appears to be confined to the top portion of the loop. This requires a suppression of conduction within the source region. Combining imaging spectroscopic observations of RHESSI with the GOES light curves, we model the evolution of the loops in the gradual phase of several flares. We find that the suppression of conduction alone can not account for the RHESSI observations in a quasi-steady equilibrium loop model. A sustained (although declining) energy input is also needed. Thermal damping of turbulence produced continuously (albeit at a declining rate) during the decay phase can be responsible for the heating process. Presence of turbulence could also suppress the conduction rate. This work is supported by NASA grants NAG5-12111, NAG5 11918-1, and NSF grant ATM-0312344.

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