Nonstationary magnetorotational processes in a rotating magnetized cloud

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dc.creatorArdeljan, N. V.
dc.creatorBisnovatyi-Kogan, G. S.
dc.creatorMoiseenko, S. G.
dc.date1999-12-24
dc.date.accessioned2026-07-07T02:35:12Z
dc.date.available2026-07-07T02:35:12Z
dc.descriptionWe perform 2D numerical simulations of a magnetorotational explosion of a rotating magnetized gas cloud. We found that amplification of a toroidal magnetic field due to the differential rotation leads to a transformation of the part of the rotational energy of the cloud to the radial kinetic energy. Simulations have been made for 3 initial values of $ξ$ (the relation of magnetic energy to the gravitational energy of the cloud): $ξ=10^{-2},10^{-4},10^{-6}$. Part of the matter - $\sim 7%$ of the mass of the cloud ($\sim 3.3%$ of the final gravitational energy of the cloud) - gets radial kinetic energy which is larger than its potential energy and can be thrown away to the infinity. It carries about 30% of the initial angular momentum of the cloud. This effect is important for angular momentum loss in the processes of stellar formation, and for the magnetorotational mechanism of explosion suggested for supernovae. Simulations have been made on the basis of the Lagrangian 2D numerical implicit scheme on a triangular grid with grid reconstruction.
dc.description11 pages, 25 figures, Accepted for publication in A&A
dc.identifierhttps://arxiv.org/abs/astro-ph/9912513
dc.identifierhttp://arxiv.org/abs/astro-ph/9912513
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/15525
dc.subjectAstrophysics
dc.titleNonstationary magnetorotational processes in a rotating magnetized cloud
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