Two-fluid Numerical Simulations of the Origin of the Fast Solar Wind

D. Wójcik; B. Kuźma; K. Murawski; A. K. Srivastava

doi:10.3847/1538-4357/ab26b1

Two-fluid Numerical Simulations of the Origin of the Fast Solar Wind

D. Wójcik
, B. Kuźma
, K. Murawski
, A. K. Srivastava

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

21 Scopus citations

Abstract

With the use of our JOANNA code, which solves radiative equations for ion + electron and neutral fluids, we perform realistic 2.5D numerical simulations of plasma outflows associated with the solar granulation. These outflows exhibit physical quantities that are consistent, to the order of magnitude, with the observational findings for mass and energy losses in the upper chromosphere, transition region, and inner corona, and they may originate the fast solar wind.

Original language	English
Article number	127
Journal	Astrophysical Journal
Volume	884
Issue number	2
DOIs	https://doi.org/10.3847/1538-4357/ab26b1
State	Published - 20 Oct 2019
Externally published	Yes

Keywords

Sun: activity
Sun: corona
magnetohydrodynamics (MHD)
methods: numerical
solar wind

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10.3847/1538-4357/ab26b1

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title = "Two-fluid Numerical Simulations of the Origin of the Fast Solar Wind",

abstract = "With the use of our JOANNA code, which solves radiative equations for ion + electron and neutral fluids, we perform realistic 2.5D numerical simulations of plasma outflows associated with the solar granulation. These outflows exhibit physical quantities that are consistent, to the order of magnitude, with the observational findings for mass and energy losses in the upper chromosphere, transition region, and inner corona, and they may originate the fast solar wind.",

keywords = "Sun: activity, Sun: corona, magnetohydrodynamics (MHD), methods: numerical, solar wind",

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AU - Wójcik, D.

AU - Kuźma, B.

AU - Murawski, K.

AU - Srivastava, A. K.

PY - 2019/10/20

Y1 - 2019/10/20

N2 - With the use of our JOANNA code, which solves radiative equations for ion + electron and neutral fluids, we perform realistic 2.5D numerical simulations of plasma outflows associated with the solar granulation. These outflows exhibit physical quantities that are consistent, to the order of magnitude, with the observational findings for mass and energy losses in the upper chromosphere, transition region, and inner corona, and they may originate the fast solar wind.

AB - With the use of our JOANNA code, which solves radiative equations for ion + electron and neutral fluids, we perform realistic 2.5D numerical simulations of plasma outflows associated with the solar granulation. These outflows exhibit physical quantities that are consistent, to the order of magnitude, with the observational findings for mass and energy losses in the upper chromosphere, transition region, and inner corona, and they may originate the fast solar wind.

KW - Sun: activity

KW - Sun: corona

KW - magnetohydrodynamics (MHD)

KW - methods: numerical

KW - solar wind

UR - https://www.scopus.com/pages/publications/85075190045

U2 - 10.3847/1538-4357/ab26b1

DO - 10.3847/1538-4357/ab26b1

M3 - 文章

AN - SCOPUS:85075190045

SN - 0004-637X

VL - 884

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

M1 - 127

ER -

Two-fluid Numerical Simulations of the Origin of the Fast Solar Wind

Abstract

Keywords

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