Realistic 3D MHD modeling of self-organized magnetic structuring of the solar corona

Document Type

Conference Proceeding

Publication Date

1-1-2020

Abstract

The dynamics of solar magnetoconvection spans a wide range of spatial and temporal scales and extends from the interior to the corona. Using 3D radiative MHD simulations, we investigate the complex interactions that drive various phenomena observed on the solar surface, in the low atmosphere, and in the corona. We present results of our recent simulations of coronal dynamics driven by underlying magnetoconvection and atmospheric processes, using the 3D radiative MHD code StellarBox (Wray et al. 2018). In particular, we focus on the evolution of thermodynamic properties and energy exchange across the different layers from the solar interior to the corona.

Identifier

85093957827 (Scopus)

Publication Title

Proceedings of the International Astronomical Union

External Full Text Location

https://doi.org/10.1017/S1743921320001532

e-ISSN

17439221

ISSN

17439213

First Page

346

Last Page

350

Issue

354

Volume

15

Grant

NNX12AD05A

Fund Ref

National Aeronautics and Space Administration

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