Flux Ropes in the Magnetic Solar Convection Zone: Numerical Simulations

Details Flux Ropes in the Magnetic Solar Convection Zone: Numerical Simulations Flux Ropes in the Magnetic Solar Convection Zone: Numerical Simulations

Aug 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd...3e...8d&link_type=abstract

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

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Scientific paper

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.

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