Please use this identifier to cite or link to this item: http://hdl.handle.net/10995/102058
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dc.contributor.authorKhaibrakhmanov, S. A.en
dc.contributor.authorDudorov, A. E.en
dc.date.accessioned2021-08-31T15:01:35Z-
dc.date.available2021-08-31T15:01:35Z-
dc.date.issued2017-
dc.identifier.citationKhaibrakhmanov S. A. Magnetic field buoyancy in accretion disks of young stars / S. A. Khaibrakhmanov, A. E. Dudorov. — DOI 10.1134/S1547477117060176 // Physics of Particles and Nuclei Letters. — 2017. — Vol. 14. — Iss. 6. — P. 882-885.en
dc.identifier.issn15474771-
dc.identifier.otherFinal2
dc.identifier.otherAll Open Access, Green3
dc.identifier.otherhttps://www.scopus.com/inward/record.uri?eid=2-s2.0-85036519100&doi=10.1134%2fS1547477117060176&partnerID=40&md5=893d78ba2f5e64e73294a35a83bb8bc6
dc.identifier.otherhttp://arxiv.org/pdf/1712.10148m
dc.identifier.urihttp://hdl.handle.net/10995/102058-
dc.description.abstractBuoyancy of the fossil magnetic field in the accretion disks of young stars is investigated. It is assumed that the Parker instability leads to the formation of slender flux tubes of toroidal magnetic field in the regions of effective magnetic field generation. Stationary solution of the induction equation is written in the form in which the buoyancy is treated as the additional mechanism of the magnetic flux escape. We calculate the fossil magnetic field intensity in the accretion disks of young T Tauri stars for the cases when radius of the magnetic flux tubes amft = 0.1H,0.5H or 1H, where H is the accretion disk height scale. Calculations show that the buoyancy limits toroidal magnetic field growth, so that its strength is comparable with the vertical magnetic field strength for the case amft = 0.1H. © 2017, Pleiades Publishing, Ltd.en
dc.format.mimetypeapplication/pdfen
dc.language.isoenen
dc.publisherMaik Nauka Publishing / Springer SBMen
dc.rightsinfo:eu-repo/semantics/openAccessen
dc.sourcePhys. Part. Nucl. Lett.2
dc.sourcePhysics of Particles and Nuclei Lettersen
dc.titleMagnetic field buoyancy in accretion disks of young starsen
dc.typeArticleen
dc.typeinfo:eu-repo/semantics/articleen
dc.typeinfo:eu-repo/semantics/publishedVersionen
dc.identifier.doi10.1134/S1547477117060176-
dc.identifier.scopus85036519100-
local.contributor.employeeKhaibrakhmanov, S.A., Kourovka Astronomical Observatory, Ural Federal University, Ekaterinburg, 620000, Russian Federation, Theoretical Physics Department, Chelyabinsk State University, Chelyabinsk, 454001, Russian Federation
local.contributor.employeeDudorov, A.E., Theoretical Physics Department, Chelyabinsk State University, Chelyabinsk, 454001, Russian Federation
local.description.firstpage882-
local.description.lastpage885-
local.issue6-
local.volume14-
local.contributor.departmentKourovka Astronomical Observatory, Ural Federal University, Ekaterinburg, 620000, Russian Federation
local.contributor.departmentTheoretical Physics Department, Chelyabinsk State University, Chelyabinsk, 454001, Russian Federation
local.identifier.pure6176621-
local.identifier.eid2-s2.0-85036519100-
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