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

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

Research output: Contribution to journal › Conference article › peer-review

1 Scopus citations

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
Volume	15
Issue number	354
DOIs	https://doi.org/10.1017/S1743921320001532
State	Published - 2020
Event	354th Symposium of the International Astronomical Union on Solar and Stellar Magnetic Fields: Origins and Manifestations - Copiapo, Chile Duration: Jun 30 2019 → Jul 6 2019

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

Keywords

(magnetohydrodynamics:) MHD
Sun: corona, magnetic fields
Sun: transition region
convection
methods: numerical
plasmas
shock waves
turbulence
waves

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10.1017/S1743921320001532

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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, Sun: corona, magnetic fields, Sun: transition region, convection, methods: numerical, plasmas, shock waves, turbulence, waves",

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

note = "Publisher Copyright: {\textcopyright} International Astronomical Union, 2020.; 354th Symposium of the International Astronomical Union on Solar and Stellar Magnetic Fields: Origins and Manifestations ; Conference date: 30-06-2019 Through 06-07-2019",

year = "2020",

doi = "10.1017/S1743921320001532",

language = "English (US)",

volume = "15",

pages = "346--350",

journal = "Proceedings of the International Astronomical Union",

issn = "1743-9213",

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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.

N1 - Publisher Copyright: © International Astronomical Union, 2020.

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 - Sun: corona, magnetic fields

KW - Sun: transition region

KW - convection

KW - methods: numerical

KW - plasmas

KW - shock waves

KW - turbulence

KW - waves

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JO - Proceedings of the International Astronomical Union

JF - Proceedings of the International Astronomical Union

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T2 - 354th Symposium of the International Astronomical Union on Solar and Stellar Magnetic Fields: Origins and Manifestations

Y2 - 30 June 2019 through 6 July 2019

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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