Ref: CTALK-2019-0001

Simulation of dynamics of hot plasma in postflare loops

Shestov, S ; Zhukov, A ; Van Doorsselaere, T

Talk presented at SDO 2018 Science Workshop on 2018-10-31

Abstract: We investigate dynamics of hot plasma in postflare coronal loops using state of the art MHD modeling and calculating synthetic images/fluxes in various SDO channels and other spectral bands – GOES and Mg XII 8.42 A spectral line. Our aim is to investigate dynamics of evaporation and condensation/draining of hot plasma in postflare loops. We use 2D and 3D MHD simulations, start with loop-like initial magnetic field and realistic plasma parameters. For the solving of MHD equations we use MPI-AMRVAC code with gravity, thermal conduction and radiative loses. We apply arbitrary heating in the chromosphere which mimic chromospheric heating by the energetic electrons from the reconnection region. The plasma starts to evaporate and soon fills the overlying magnetic loop system. The particular observed characteristics –, temperature, density, flow, and their dynamics strongly depend on applied physical condition. In particular, strength of magnetic field plays important role, as well as heating rate and the size of the heated region. To constrain the possible range of parameters we calculate synthetic images/fluxes in various EUV and X-ray channels with the use of FoMo code. We compare calculated images with observational data (we chose one large-scale and one small-scale loop associated with ~B-class flares) and identify the most probable physical conditions, in which synthetic data match observations. We were able to find heating regimes to match the observations; beside we see several interesting features that can be revealed only in 2D or 3D modeling.


The record appears in these collections:
Conference Contributions & Seminars > Conference Talks > Contributed Talks
Royal Observatory of Belgium > Solar Physics & Space Weather (SIDC)
Solar-Terrestrial Centre of Excellence

 Record created 2019-01-08, last modified 2019-01-08