Three-dimensional modeling of mass transfer in close binary systems with non-synchronous rotation

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dc.creatorBisikalo, D. V.
dc.creatorBoyarchuk, A. A.
dc.creatorKuznetsov, O. A.
dc.creatorChechetkin, V. M.
dc.date1998-12-31
dc.date.accessioned2026-07-07T02:29:51Z
dc.date.available2026-07-07T02:29:51Z
dc.descriptionWe present the results of three-dimensional numerical simulations of mass transfer in semi-detached binary systems in which the mass-losing star is rotating. The cases of aligned and misaligned non-synchronous rotation of the donor star are considered; the resulting flow patterns are compared to the synchronous case. The main properties of the flow, such as the formation of an circumbinary envelope, the absence of a "hot spot" on the edge of the accretion disk, and the formation of a shock wave along the flow edge, are qualitatively similar to those obtained earlier. For the case of misaligned, non-synchronous rotation, the behavior of the disk and surrounding matter in established flow regime reflects changes in the boundary conditions at the surface of the donor star; in other words, a "driven disk" model is realized in the calculations.
dc.descriptionLaTeX, 22 pages, accepted for publication in Astronomy Reports
dc.identifierhttps://arxiv.org/abs/astro-ph/9812484
dc.identifierhttp://arxiv.org/abs/astro-ph/9812484
dc.identifierAstron. Zh. 1999, v.76, p.270 (Astron. Reports v.43, p.229)
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/13634
dc.subjectAstrophysics
dc.titleThree-dimensional modeling of mass transfer in close binary systems with non-synchronous rotation
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