Please use this identifier to cite or link to this item: http://elar.urfu.ru/handle/10995/101946
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dc.contributor.authorKhaibrakhmanov, S. A.en
dc.contributor.authorDudorov, A.en
dc.contributor.authorSobolev, A.en
dc.date.accessioned2021-08-31T15:00:49Z-
dc.date.available2021-08-31T15:00:49Z-
dc.date.issued2018-
dc.identifier.citationKhaibrakhmanov S. Dynamics of magnetic flux tubes and IR-variability of young stellar objects / S. Khaibrakhmanov, A. Dudorov, A. Sobolev. — DOI 10.1088/1674-4527/18/8/90 // Research in Astronomy and Astrophysics. — 2018. — Vol. 18. — Iss. 8. — 090.en
dc.identifier.issn16744527-
dc.identifier.otherFinal2
dc.identifier.otherAll Open Access, Green3
dc.identifier.otherhttps://www.scopus.com/inward/record.uri?eid=2-s2.0-85051504825&doi=10.1088%2f1674-4527%2f18%2f8%2f90&partnerID=40&md5=08940ba0afa5e8a1e3345927a2efcbe5
dc.identifier.otherhttp://arxiv.org/pdf/1712.09094m
dc.identifier.urihttp://elar.urfu.ru/handle/10995/101946-
dc.description.abstractWe simulate the dynamics of slender magnetic flux tubes (MFTs) in the accretion disks of T Tauri stars. The dynamical equations of our model take into account aerodynamic and turbulent drag forces, and the radiative heat exchange between the MFT and ambient gas. The structure of the disk is calculated with the help of our MHD model of the accretion disks. We consider the MFTs formed at distances of 0.027-0.8 au from the star with various initial radii and plasma betas β 0. The simulations show that MFTs with a weak magnetic field (β 0 = 10) rise slowly with speeds less than the speed of sound. MFTs with β 0 = 1 form an outflowing magnetized corona above the disk. Strongly magnetized MFTs (β 0 = 0.1) can cause outflows with velocities 20 - 50 km s-1. The tubes rise periodically over times from several days to several months according to our simulations. We propose that periodically rising MFTs can absorb stellar radiation and contribute to the IR-variability of young stellar objects. © 2018 National Astronomical Observatories, CAS and IOP Publishing Ltd..en
dc.format.mimetypeapplication/pdfen
dc.language.isoenen
dc.publisherInstitute of Physics Publishingen
dc.rightsinfo:eu-repo/semantics/openAccessen
dc.sourceRes. Astron. Astrophys.2
dc.sourceResearch in Astronomy and Astrophysicsen
dc.subjectACCRETION DISKSen
dc.subjectINSTABILITIESen
dc.subjectMAGNETOHYDRODYNAMICS (MHD)en
dc.subjectPROTOPLANETARY DISKSen
dc.titleDynamics of magnetic flux tubes and IR-variability of young stellar objectsen
dc.typeConference Paperen
dc.typeinfo:eu-repo/semantics/conferenceObjecten
dc.typeinfo:eu-repo/semantics/publishedVersionen
dc.identifier.rsi35726406-
dc.identifier.doi10.1088/1674-4527/18/8/90-
dc.identifier.scopus85051504825-
local.contributor.employeeKhaibrakhmanov, S., Kourovka Astronomical Observatory, Ural Federal University, Ekaterinburg, 620000, Russian Federation, Theoretical Physics Department, Chelyabinsk State University, Chelyabinsk, 454001, Russian Federation
local.contributor.employeeDudorov, A., Theoretical Physics Department, Chelyabinsk State University, Chelyabinsk, 454001, Russian Federation
local.contributor.employeeSobolev, A., Kourovka Astronomical Observatory, Ural Federal University, Ekaterinburg, 620000, Russian Federation
local.issue8-
local.volume18-
dc.identifier.wos000441296300003-
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.puredf76b98e-769f-431e-994e-48f2004d1a04uuid
local.identifier.pure7760088-
local.description.order090-
local.identifier.eid2-s2.0-85051504825-
local.identifier.wosWOS:000441296300003-
Appears in Collections:Научные публикации ученых УрФУ, проиндексированные в SCOPUS и WoS CC

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