Flux ropes in the magnetic solar convection zone: Numerical simulations

S. B. F. Dorch

Flux ropes in the magnetic solar convection zone: Numerical simulations

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Research output: Contribution to journal › Journal article › Research

Abstract

In this contribution results are presented on how twisted magnetic flux ropes interact with a magnetized model envelope similar to the solar convection zone. Both the flux ropes and the atmosphere are modelled as idealized 2.5-dimensional concepts using high resolution numerical MHD simulations (on meshes of over 4 million grid points): A uniformly twisted buoyant "toroidal" flux rope is placed near the bottom of an adiabatically stratified atmosphere. Inside the atmosphere a "poloidal" magnetic layer is placed, into which the flux rope ascends. It is shown that the twisted magnetic field of the magnetic flux ropes interact with the magnetic field in the atmosphere in a manner that depends, among other things, on the polarity and strength of the atmospheric field. The results include limits on the necessary and possible twist and polarity of solar magnetic flux ropes.

Original language	English
Journal	Solar Active Regions and 3D Magnetic Structure, 26th meeting of the IAU, Joint Discussion 3, 16-17 August, 2006, Prague, Czech Republic, JD03, #8
Volume	3
Pages (from-to)	8
Publication status	Published - 2006
Externally published	Yes

Documents & Links

http://adsabs.harvard.edu/abs/2006IAUJD...3E...8D

MAGSTAR: Research Theme 1: Astrophysical and stellar magnetism
Dorch, B., Nordlund, Å., Freytag, B., Archontis, V., Gudiksen, B. V. & Christensen, M. B. E.
10/04/2002 → …
Project: Research

Cite this

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title = "Flux ropes in the magnetic solar convection zone: Numerical simulations",

abstract = "In this contribution results are presented on how twisted magnetic flux ropes interact with a magnetized model envelope similar to the solar convection zone. Both the flux ropes and the atmosphere are modelled as idealized 2.5-dimensional concepts using high resolution numerical MHD simulations (on meshes of over 4 million grid points): A uniformly twisted buoyant {"}toroidal{"} flux rope is placed near the bottom of an adiabatically stratified atmosphere. Inside the atmosphere a {"}poloidal{"} magnetic layer is placed, into which the flux rope ascends. It is shown that the twisted magnetic field of the magnetic flux ropes interact with the magnetic field in the atmosphere in a manner that depends, among other things, on the polarity and strength of the atmospheric field. The results include limits on the necessary and possible twist and polarity of solar magnetic flux ropes.",

author = "Dorch, {S. B. F.}",

year = "2006",

language = "English",

volume = "3",

pages = "8",

journal = "Solar Active Regions and 3D Magnetic Structure, 26th meeting of the IAU, Joint Discussion 3, 16-17 August, 2006, Prague, Czech Republic, JD03, #8",

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TY - JOUR

T1 - Flux ropes in the magnetic solar convection zone

T2 - Numerical simulations

AU - Dorch, S. B. F.

PY - 2006

Y1 - 2006

N2 - In this contribution results are presented on how twisted magnetic flux ropes interact with a magnetized model envelope similar to the solar convection zone. Both the flux ropes and the atmosphere are modelled as idealized 2.5-dimensional concepts using high resolution numerical MHD simulations (on meshes of over 4 million grid points): A uniformly twisted buoyant "toroidal" flux rope is placed near the bottom of an adiabatically stratified atmosphere. Inside the atmosphere a "poloidal" magnetic layer is placed, into which the flux rope ascends. It is shown that the twisted magnetic field of the magnetic flux ropes interact with the magnetic field in the atmosphere in a manner that depends, among other things, on the polarity and strength of the atmospheric field. The results include limits on the necessary and possible twist and polarity of solar magnetic flux ropes.

AB - In this contribution results are presented on how twisted magnetic flux ropes interact with a magnetized model envelope similar to the solar convection zone. Both the flux ropes and the atmosphere are modelled as idealized 2.5-dimensional concepts using high resolution numerical MHD simulations (on meshes of over 4 million grid points): A uniformly twisted buoyant "toroidal" flux rope is placed near the bottom of an adiabatically stratified atmosphere. Inside the atmosphere a "poloidal" magnetic layer is placed, into which the flux rope ascends. It is shown that the twisted magnetic field of the magnetic flux ropes interact with the magnetic field in the atmosphere in a manner that depends, among other things, on the polarity and strength of the atmospheric field. The results include limits on the necessary and possible twist and polarity of solar magnetic flux ropes.

M3 - Journal article

VL - 3

SP - 8

JO - Solar Active Regions and 3D Magnetic Structure, 26th meeting of the IAU, Joint Discussion 3, 16-17 August, 2006, Prague, Czech Republic, JD03, #8

JF - Solar Active Regions and 3D Magnetic Structure, 26th meeting of the IAU, Joint Discussion 3, 16-17 August, 2006, Prague, Czech Republic, JD03, #8

ER -

Flux ropes in the magnetic solar convection zone: Numerical simulations

Abstract

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MAGSTAR: Research Theme 1: Astrophysical and stellar magnetism

Cite this