Two-dimensional MHD simulation for prominence eruption with radiative condensation
Abstract
We reproduced solar prominence eruption using 2.5-dimensional magnetohydrodynamic (MHD) simulations including nonlinear anisotropic thermal conduction and optically thin radiative cooling. Solar prominence eruption is a progenitor of coronal mass ejection and one of the important subjects in studies of solar physics and space weather. Only a few numerical simulation have been carried out for prominence eruptions due to difficulty in reproducing cool dense plasmas of prominence in the hot tenuous corona. In this study, we numerically modeled prominence eruption by combining prominence formation model (Kaneko & Yokoyama, 2015, 2017) and flare trigger model (Kusano et al., 2012). In the present simulations, a flux rope is created by reconnections between coronal arcade fields and a newly emerging bipole. Radiative condensation is triggered inside the flux rope, leading to prominence formation. The flux rope hosting prominence erupts by MHD instability and reconnection. As a result of parameter survey, we found that momentum as well as mass in the coronal flux rope is condensed into prominence, facilitating the initiation of MHD instability responsible for eruptions. Our results suggest that the slow rise phase of prominence eruptions is maintained or extended by momentum condensation from the corona toward prominence.
- Publication:
-
42nd COSPAR Scientific Assembly
- Pub Date:
- July 2018
- Bibcode:
- 2018cosp...42E1674K