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dc.contributor.authorKargaltseva, N. S.en
dc.contributor.authorKhaibrakhmanov, S. A.en
dc.contributor.authorDudorov, A. E.en
dc.contributor.authorZamozdra, S. N.en
dc.contributor.authorZhilkin, A. G.en
dc.date.accessioned2022-10-19T05:19:58Z-
dc.date.available2022-10-19T05:19:58Z-
dc.date.issued2022-
dc.identifier.citationInfluence of the magnetic field on the formation of protostellar disks / N. S. Kargaltseva, S. A. Khaibrakhmanov, A. E. Dudorov et al. // Open Astronomy. — 2022. — Vol. 31. — Iss. 1. — P. 172-180.en
dc.identifier.issn25436376-
dc.identifier.otherhttps://www.scopus.com/inward/record.uri?eid=2-s2.0-85129113018&doi=10.1515%2fastro-2022-0022&partnerID=40&md5=e9243fcabb16e309a70c05e80847c90dlink
dc.identifier.urihttp://elar.urfu.ru/handle/10995/117855-
dc.description.abstractWe numerically model the collapse of magnetic rotating protostellar clouds with mass of 10 M The simulations are carried out with the help of 2D MHD code Enlil. The structure of the cloud at the isothermal stage of the collapse is investigated for the cases of weak, moderate, and strong initial magnetic field. Simulations reveal the universal hierarchical structure of collapsing protostellar clouds, consisting of the flattened envelope with the qausi-magnetostatc disk inside and the first core in its center. The size of the primary disk increases with the initial magnetic energy of the cloud. The magnetic braking efficiently transports the angular momentum from the primary disk into the envelope in the case, when the initial magnetic energy of the cloud is more than 20% of its gravitational energy. The intensity of the outflows launched from the region near the boundary of the first core increases with initial magnetic energy. The "dead"zone with small ionization fraction, x < 1 0-11 x< 1{0){-11}, forms inside the first hydrostatic core and at the base of the outflow. Ohmic dissipation and ambipolar diffusion determine conditions for further formation of the protostellar disk in this region. © 2022 Natalya S. Kargaltseva et al., published by De Gruyter.en
dc.description.sponsorshipRussian Science Foundation, RSF: 19-72-10012en
dc.description.sponsorshipFunding information: This work is financially supported by the Russian Science Foundation (project 19-72-10012).en
dc.format.mimetypeapplication/pdfen
dc.language.isoenen
dc.publisherDe Gruyter Open Ltden
dc.relationinfo:eu-repo/grantAgreement/RSF//19-72-10012en
dc.rightsinfo:eu-repo/semantics/openAccessen
dc.sourceOpen Astronomyen
dc.subjectINTERSTELLAR MEDIUMen
dc.subjectMAGNETIC FIELDSen
dc.subjectMAGNETIC-GAS-DYNAMICSen
dc.subjectNUMERICAL SIMULATIONen
dc.subjectSTAR FORMATIONen
dc.titleInfluence of the magnetic field on the formation of protostellar disksen
dc.typeArticleen
dc.typeinfo:eu-repo/semantics/articleen
dc.typeinfo:eu-repo/semantics/publishedVersionen
dc.identifier.doi10.1515/astro-2022-0022-
dc.identifier.scopus85129113018-
local.contributor.employeeKargaltseva, N.S., Chelyabinsk State University, Department of General and Theoretical Physics, 129 Br. Kashirinykh str., Chelyabinsk, 454001, Russian Federation, Ural Federal University, Kourovka Astronomical Observatory, 51 Lenina str., Ekaterinburg, 620000, Russian Federationen
local.contributor.employeeKhaibrakhmanov, S.A., Chelyabinsk State University, Department of General and Theoretical Physics, 129 Br. Kashirinykh str., Chelyabinsk, 454001, Russian Federation, Ural Federal University, Kourovka Astronomical Observatory, 51 Lenina str., Ekaterinburg, 620000, Russian Federationen
local.contributor.employeeDudorov, A.E., Chelyabinsk State University, Department of General and Theoretical Physics, 129 Br. Kashirinykh str., Chelyabinsk, 454001, Russian Federation, Ural Federal University, Kourovka Astronomical Observatory, 51 Lenina str., Ekaterinburg, 620000, Russian Federationen
local.contributor.employeeZamozdra, S.N., Chelyabinsk State University, Department of General and Theoretical Physics, 129 Br. Kashirinykh str., Chelyabinsk, 454001, Russian Federationen
local.contributor.employeeZhilkin, A.G., Institute of Astronomy of the Russian Academy of Sciences (INASAN), Department of Stellar Physics and Evolution, Moscow, 119017, Russian Federationen
local.description.firstpage172-
local.description.lastpage180-
local.issue1-
local.volume31-
dc.identifier.wos000786710100001-
local.contributor.departmentChelyabinsk State University, Department of General and Theoretical Physics, 129 Br. Kashirinykh str., Chelyabinsk, 454001, Russian Federationen
local.contributor.departmentUral Federal University, Kourovka Astronomical Observatory, 51 Lenina str., Ekaterinburg, 620000, Russian Federationen
local.contributor.departmentInstitute of Astronomy of the Russian Academy of Sciences (INASAN), Department of Stellar Physics and Evolution, Moscow, 119017, Russian Federationen
local.identifier.pure30099862-
local.identifier.eid2-s2.0-85129113018-
local.fund.rsf19-72-10012-
local.identifier.wosWOS:000786710100001-
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