Flux ropes in the magnetic solar convection zone: Numerical simulations

Research output: Contribution to journalJournal articleResearch


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 languageEnglish
JournalSolar Active Regions and 3D Magnetic Structure, 26th meeting of the IAU, Joint Discussion 3, 16-17 August, 2006, Prague, Czech Republic, JD03, #8
Pages (from-to)8
Publication statusPublished - 2006
Externally publishedYes


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