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

Irina N. Kitiashvili; Alan A. Wray; Viacheslav Sadykov; Alexander G. Kosovichev; Nagi N. Mansour; Alexander Kosovichev; Klaus Strassmeier; Moira Jardine

doi:10.1017/S1743921320001532

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

Irina N. Kitiashvili, Alan A. Wray, Viacheslav Sadykov, Alexander G. Kosovichev, Nagi N. Mansour, Alexander Kosovichev, Klaus Strassmeier, Moira Jardine

Research output: Contribution to journal › Article › peer-review

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.

Original language	English (US)
Pages (from-to)	346-350
Number of pages	5
Journal	Proceedings of the International Astronomical Union
DOIs	https://doi.org/10.1017/S1743921320001532
State	Accepted/In press - 2020

All Science Journal Classification (ASJC) codes

Medicine (miscellaneous)
Astronomy and Astrophysics
Nutrition and Dietetics
Public Health, Environmental and Occupational Health
Space and Planetary Science

Keywords

(magnetohydrodynamics:) MHD
convection
methods: Numerical
plasmas
shock waves
Sun: Corona, magnetic fields
Sun: Transition region
turbulence
waves

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10.1017/S1743921320001532

Cite this

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title = "Realistic 3D MHD modeling of self-organized magnetic structuring of the solar corona",

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. ",

keywords = "(magnetohydrodynamics:) MHD, convection, methods: Numerical, plasmas, shock waves, Sun: Corona, magnetic fields, Sun: Transition region, turbulence, waves",

author = "Kitiashvili, {Irina N.} and Wray, {Alan A.} and Viacheslav Sadykov and Kosovichev, {Alexander G.} and Mansour, {Nagi N.} and Alexander Kosovichev and Klaus Strassmeier and Moira Jardine",

year = "2020",

doi = "10.1017/S1743921320001532",

language = "English (US)",

pages = "346--350",

journal = "Proceedings of the International Astronomical Union",

issn = "1743-9213",

publisher = "Cambridge University Press",

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TY - JOUR

T1 - Realistic 3D MHD modeling of self-organized magnetic structuring of the solar corona

AU - Kitiashvili, Irina N.

AU - Wray, Alan A.

AU - Sadykov, Viacheslav

AU - Kosovichev, Alexander G.

AU - Mansour, Nagi N.

AU - Kosovichev, Alexander

AU - Strassmeier, Klaus

AU - Jardine, Moira

PY - 2020

Y1 - 2020

N2 - 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.

AB - 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.

KW - (magnetohydrodynamics:) MHD

KW - convection

KW - methods: Numerical

KW - plasmas

KW - shock waves

KW - Sun: Corona, magnetic fields

KW - Sun: Transition region

KW - turbulence

KW - waves

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JO - Proceedings of the International Astronomical Union

JF - Proceedings of the International Astronomical Union

SN - 1743-9213

ER -

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

Abstract

All Science Journal Classification (ASJC) codes

Keywords

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