Evolution of Collapse Nonuniformity for Rotating Magnetic Interstellar Clouds

Simple item page
dc.creatorDudorov, A. E.
dc.creatorZhilkin, A. G.
dc.creatorZhilkina, N. Y.
dc.date2006-07-26
dc.date.accessioned2026-07-07T07:15:46Z
dc.date.available2026-07-07T07:15:46Z
dc.descriptionWe investigate the formation and evolution of isothermal collapse nonuniformity for rotating magnetic interstellar clouds. The initial and boundary conditions correspond to the statement of the problem of homogeneous cloud contraction from a pressure equilibrium with the external medium. The initial uniform magnetic field is collinear with the angular velocity. Fast and slow magnetosonic rarefaction waves are shown to be formed and propagate from the boundary of the cloud toward its center in the early collapse stages. The front of the fast rarefaction wave divides the gas mass into two parts. The density, angular velocity, and magnetic field remain uniform in the inner region and have nonuniform profiles in the outer region. The rarefaction wave front surface can take both prolate and oblate shapes along the rotation axis, depending on the relationship between the initial angular velocity and magnetic field. We derive a criterion that separates the two regimes of rarefaction wave dynamics with the dominant role of electromagnetic and centrifugal forces. Based on analytical estimations and numerical calculations, we discuss possible scenarios for the evolution of collapse nonuniformity for rotating magnetic interstellar clouds.
dc.description19 pages, 7 figures, submitted in Astronomy Letters, 2006, 32, 9, 622-632
dc.identifierhttps://arxiv.org/abs/astro-ph/0607588
dc.identifierhttp://arxiv.org/abs/astro-ph/0607588
dc.identifierAstron.Lett. 32 (2006) 622-632
dc.identifierdoi:10.1134/S1063773706090076
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/113338
dc.subjectAstrophysics
dc.titleEvolution of Collapse Nonuniformity for Rotating Magnetic Interstellar Clouds
dc.typetext

Files

Collections

arXiv