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Formation of Solar Filaments by Steady and Nonsteady Chromospheric Heating View all abstracts by submitter

Chun Xia   Submitted: 2011-05-31 23:38

It has been established that cold plasma condensations can form in a magneticloop subject to localized heating of the footpoints. In this paper, we usegrid-adaptive numerical simulations of the radiative hydrodynamic equations toparametrically investigate the filament formation process in a pre-shaped loopwith both steady and finite-time chromospheric heating. Compared to previousworks, we consider low-lying loops with shallow dips, and use a more realisticdescription for the radiative losses. We demonstrate for the first time thatthe onset of thermal instability satisfies the linear instability criterion.The onset time of the condensation is roughly sim 2 hr or more after thelocalized heating at the footpoint is effective, and the growth rate of thethread length varies from 800 km hr-1 to 4000 km hr-1, depending on theamplitude and the decay length scale characterizing this localizedchromospheric heating. We show how single or multiple condensation segments mayform in the coronal portion. In the asymmetric heating case, when two segmentsform, they approach and coalesce, and the coalesced condensation later drainsdown into the chromosphere. With a steady heating, this process repeats with aperiodicity of several hours. While our parametric survey confirms and augmentsearlier findings, we also point out that steady heating is not necessary tosustain the condensation. Once the condensation is formed, it can keep growingalso when the localized heating ceases. Finally, we show that the condensationcan survive continuous buffeting by perturbations resulting from thephotospheric p-mode waves.

Authors: C. Xia, P. F. Chen, R. Keppens, A. J. van Marle

Publication Status: ApJ(accepted)
Last Modified: 2011-06-01 21:19
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