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: http://star.arm.ac.uk/slides/aks/
Дата изменения: Wed Jun 30 13:09:26 2010 Дата индексирования: Tue Oct 2 01:47:56 2012 Кодировка: Поисковые слова: п п п п п п п п п п п |
Abstract
The magneto-convection of the plasma in solar and stellar
convection zones are very important to carry the heat and magnetic
fluxes at the surface. The anelastic approximation has strong advantages
for the numerical simulation of stellar and solar convection zones, and
model the dynamics of buoyant magnetic flux tubes emerging in the
solar/stellar atmospheres from their interior. This approximation
suppressed the acoustic modes and permits the larger simulated time
steps that will not be possible in fully compressible models. In the
first part, I'll describe the basic physical model of solar convection
zone and the scenario of MLT theory and anelastic approximation .
While, I'll discuss the computational techniques related to anelastic
MHD simulation, and its application in the second part.
Part 1 Theory - PDF format (5.3MB)
Part 2 Computation - PDF format (4.4MB)
Last Revised: 2010 June 30th |