Critical decay index at the onset of solar eruptions

F. P. Zuccarello; G. Aulanier; S. A. Gilchrist

doi:10.1088/0004-637X/814/2/126

Critical decay index at the onset of solar eruptions

F. P. Zuccarello
, G. Aulanier
, S. A. Gilchrist

Sorbonne Univ.

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

Abstract

Magnetic flux ropes are topological structures consisting of twisted magnetic field lines that globally wrap around an axis. The torus instability model predicts that a magnetic flux rope of major radius R undergoes an eruption when its axis reaches a location where the decay index of the ambient magnetic field B_ex is larger than a critical value. In the current-wire model, the critical value depends on the thickness and time.

Original language	English
Article number	126
Journal	Astrophysical Journal
Volume	814
Issue number	2
DOIs	https://doi.org/10.1088/0004-637X/814/2/126
Publication status	Published - 1 Dec 2015
Externally published	Yes

Keywords

Sun: coronal mass ejections (CMEs)
instabilities
magnetohydrodynamics (MHD)
methods: numerical

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10.1088/0004-637X/814/2/126

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title = "Critical decay index at the onset of solar eruptions",

abstract = "Magnetic flux ropes are topological structures consisting of twisted magnetic field lines that globally wrap around an axis. The torus instability model predicts that a magnetic flux rope of major radius R undergoes an eruption when its axis reaches a location where the decay index of the ambient magnetic field Bex is larger than a critical value. In the current-wire model, the critical value depends on the thickness and time.",

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AU - Aulanier, G.

AU - Gilchrist, S. A.

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AB - Magnetic flux ropes are topological structures consisting of twisted magnetic field lines that globally wrap around an axis. The torus instability model predicts that a magnetic flux rope of major radius R undergoes an eruption when its axis reaches a location where the decay index of the ambient magnetic field Bex is larger than a critical value. In the current-wire model, the critical value depends on the thickness and time.

KW - Sun: coronal mass ejections (CMEs)

KW - instabilities

KW - magnetohydrodynamics (MHD)

KW - methods: numerical

U2 - 10.1088/0004-637X/814/2/126

DO - 10.1088/0004-637X/814/2/126

M3 - Article

AN - SCOPUS:84948777188

SN - 0004-637X

VL - 814

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

M1 - 126

ER -

Critical decay index at the onset of solar eruptions

Abstract

Keywords

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