Numerical simulation of the internal plasma dynamics of post-flare loops

Details Numerical simulation of the internal plasma dynamics of post-flare loops Numerical simulation of the internal plasma dynamics of post-flare loops

2009-08-14

arxiv.org/abs/0908.2123v2

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

Accepted MNRAS, 10 pages, 14 figures, 1 table

Scientific paper

We integrate the MHD ideal equations of a slender flux tube to simulate the internal plasma dynamics of coronal post-flare loops. We study the onset and evolution of the internal plasma instability to compare with observations and to gain insight into physical processes and characteristic parameters associated with flaring events. The numerical approach uses a finite-volume Harten-Yee TVD scheme to integrate the 1D1/2 MHD equations specially designed to capture supersonic flow discontinuities. We could reproduce the observational sliding down and upwardly propagating of brightening features along magnetic threads of an event occurred on October 1st, 2001. We show that high--speed downflow perturbations, usually interpreted as slow magnetoacoustic waves, could be better interpreted as slow magnetoacoustic shock waves. This result was obtained considering adiabaticity in the energy balance equation. However, a time--dependent forcing from the basis is needed to reproduce the reiteration of the event which resembles observational patterns -commonly known as quasi--periodic pulsations (QPPs)- which are related with large scale characteristic longitudes of coherence. This result reinforces the interpretation that the QPPs are a response to the pulsational flaring activity.

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