EGU22-5546
https://doi.org/10.5194/egusphere-egu22-5546
EGU General Assembly 2022
© Author(s) 2022. This work is distributed under
the Creative Commons Attribution 4.0 License.

A simulation of flare-driven coronal rain

Wenzhi Ruan, Yuhao Zhou, and Rony Keppens
Wenzhi Ruan et al.
  • KU Leuven, Centre for mathematical Plasma Astrophysics (CmPA), Department of Mathematics, Leuven, Belgium (wenzhi.ruan@kuleuven.be)

Coronal rains are cool materials (~10,000 K) that appear at hot corona. They are frequently observed in non-flaring loops of active regions and recently observed in flaring loops at gradual phases. Hot coronal loops (~10 MK) are often produced in flare events due to magnetic reconnection. The hot flare loops gradually recover to typical coronal temperature due to thermal conduction and radiative loss, during which condensation can happen due to thermal instability. Here we demonstrate how the rains formed in a flare loop with a two-and-a-half dimensional magnetohydrodynamic simulation. We simulate a flare event from pre-flare phase all the way to gradual phase and successfully reproduce coronal rains. We find that thermal conduction and radiative losses alternately dominate the cooling of the flare loop. We find that runaway cooling and rain formation also induce the appearance of dark post-flare loop systems, as observed in extreme ultraviolet (EUV) channels.

How to cite: Ruan, W., Zhou, Y., and Keppens, R.: A simulation of flare-driven coronal rain, EGU General Assembly 2022, Vienna, Austria, 23–27 May 2022, EGU22-5546, https://doi.org/10.5194/egusphere-egu22-5546, 2022.

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