Photospheric line-tying conditions for the MHD stability of coronal magnetic fields

A. W. Hood

doi:10.1007/BF00172049

Photospheric line-tying conditions for the MHD stability of coronal magnetic fields

A. W. Hood

Applied Mathematics

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

Abstract

Using the localised, ballooning ordering, the effect of a density stratification on the ideal MHD stability of magnetic fields is investigated. It is found that, when the photospheric density is very much greater than the coronal value, the line tying conditions are best simulated by assuming that all coronal disturbances vanish at the photospheric boundary. This is commonly known as the rigid wall conditions.

Original language	English
Pages (from-to)	307-312
Journal	Solar Physics
Volume	105
DOIs	https://doi.org/10.1007/BF00172049
Publication status	Published - 1 Jun 1986

Keywords

Density Distribution
Magnetohydrodynamic Stability
Photosphere
Solar Corona
Solar Magnetic Field
Boundary Value Problems

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10.1007/BF00172049

http://adsabs.harvard.edu/abs/1986SoPh..105..307H

Cite this

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title = "Photospheric line-tying conditions for the MHD stability of coronal magnetic fields",

abstract = "Using the localised, ballooning ordering, the effect of a density stratification on the ideal MHD stability of magnetic fields is investigated. It is found that, when the photospheric density is very much greater than the coronal value, the line tying conditions are best simulated by assuming that all coronal disturbances vanish at the photospheric boundary. This is commonly known as the rigid wall conditions.",

keywords = "Density Distribution, Magnetohydrodynamic Stability, Photosphere, Solar Corona, Solar Magnetic Field, Boundary Value Problems",

author = "Hood, {A. W.}",

year = "1986",

month = jun,

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doi = "10.1007/BF00172049",

language = "English",

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TY - JOUR

T1 - Photospheric line-tying conditions for the MHD stability of coronal magnetic fields

AU - Hood, A. W.

PY - 1986/6/1

Y1 - 1986/6/1

N2 - Using the localised, ballooning ordering, the effect of a density stratification on the ideal MHD stability of magnetic fields is investigated. It is found that, when the photospheric density is very much greater than the coronal value, the line tying conditions are best simulated by assuming that all coronal disturbances vanish at the photospheric boundary. This is commonly known as the rigid wall conditions.

AB - Using the localised, ballooning ordering, the effect of a density stratification on the ideal MHD stability of magnetic fields is investigated. It is found that, when the photospheric density is very much greater than the coronal value, the line tying conditions are best simulated by assuming that all coronal disturbances vanish at the photospheric boundary. This is commonly known as the rigid wall conditions.

KW - Density Distribution

KW - Magnetohydrodynamic Stability

KW - Photosphere

KW - Solar Corona

KW - Solar Magnetic Field

KW - Boundary Value Problems

U2 - 10.1007/BF00172049

DO - 10.1007/BF00172049

M3 - Article

SN - 0038-0938

VL - 105

SP - 307

EP - 312

JO - Solar Physics

JF - Solar Physics

ER -

Photospheric line-tying conditions for the MHD stability of coronal magnetic fields

Abstract

Keywords

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