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dc.contributor.authorRyabukhina, O. L.en
dc.contributor.authorZinchenko, I. I.en
dc.contributor.authorSamal, M. R.en
dc.contributor.authorZemlyanukha, P. M.en
dc.contributor.authorLadeyschikov, D. A.en
dc.contributor.authorSobolev, A. M.en
dc.contributor.authorHenkel, C.en
dc.contributor.authorOjha, D. K.en
dc.date.accessioned2021-08-31T15:00:50Z-
dc.date.available2021-08-31T15:00:50Z-
dc.date.issued2018-
dc.identifier.citationStudy of the filamentary infrared dark cloud G192.76+00.10 in the S254-S258 OB complex / O. L. Ryabukhina, I. I. Zinchenko, M. R. Samal, et al. — DOI 10.1088/1674-4527/18/8/95 // Research in Astronomy and Astrophysics. — 2018. — Vol. 18. — Iss. 8. — 095.en
dc.identifier.issn16744527-
dc.identifier.otherFinal2
dc.identifier.otherAll Open Access, Green3
dc.identifier.otherhttps://www.scopus.com/inward/record.uri?eid=2-s2.0-85051472390&doi=10.1088%2f1674-4527%2f18%2f8%2f95&partnerID=40&md5=0fbf1f21a6e5e7cdb0609b4371a0a986
dc.identifier.otherhttp://arxiv.org/pdf/1802.08030m
dc.identifier.urihttp://elar.urfu.ru/handle/10995/101949-
dc.description.abstractWe present results of a high resolution study of the filamentary infrared dark cloud G192.76+00.10 in the S254-S258 OB complex in several molecular species tracing different physical conditions. These include three isotopologues of carbon monoxide (CO), ammonia (NH3) and carbon monosulfide (CS). The aim of this work is to study the general structure and kinematics of the filamentary cloud, and its fragmentation and physical parameters. The gas temperature is derived from the NH3 (J, K) = (1, 1), (2, 2) and 12CO(2-1) lines, and the 13CO(1-0), 13CO(2-1) emission is used to investigate the overall gas distribution and kinematics. Several dense clumps are identified from the CS(2-1) data. Values of the gas temperature lie in the range 10 - 35K, and column density N(H2) reaches the value 5.1 1022 cm-2. The width of the filament is of order 1 pc. The masses of the dense clumps range from ∼ 30 M o to ∼ 160 M o. They appear to be gravitationally unstable. Themolecular emission shows a gas dynamical coherence along the filament. The velocity pattern may indicate longitudinal collapse. © 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.subjectISM: CLOUDSen
dc.subjectISM: INDIVIDUAL OBJECTS (G192.76+00.10)en
dc.subjectISM: MOLECULESen
dc.subjectSTARS: FORMATIONen
dc.titleStudy of the filamentary infrared dark cloud G192.76+00.10 in the S254-S258 OB complexen
dc.typeConference Paperen
dc.typeinfo:eu-repo/semantics/conferenceObjecten
dc.typeinfo:eu-repo/semantics/publishedVersionen
dc.identifier.rsi35735842-
dc.identifier.doi10.1088/1674-4527/18/8/95-
dc.identifier.scopus85051472390-
local.contributor.employeeRyabukhina, O.L., Institute of Applied Physics, Russian Academy of Sciences, Nizhny Novgorod, Russian Federation, Lobachevsky State University of Nizhni Novgorod, Nizhny Novgorod, Russian Federation
local.contributor.employeeZinchenko, I.I., Institute of Applied Physics, Russian Academy of Sciences, Nizhny Novgorod, Russian Federation, Lobachevsky State University of Nizhni Novgorod, Nizhny Novgorod, Russian Federation
local.contributor.employeeSamal, M.R., Institute of Astronomy, National Central University, Taoyuan City, Taiwan
local.contributor.employeeZemlyanukha, P.M., Institute of Applied Physics, Russian Academy of Sciences, Nizhny Novgorod, Russian Federation
local.contributor.employeeLadeyschikov, D.A., Kourovka Astronomical Observatory, Ural Federal University, Ekaterinburg, Russian Federation
local.contributor.employeeSobolev, A.M., Kourovka Astronomical Observatory, Ural Federal University, Ekaterinburg, Russian Federation
local.contributor.employeeHenkel, C., Max Planck Institute for Radio Astronomy, Bonn, Germany, Astron. Dept., King Abdulaziz University, Jeddah, Saudi Arabia
local.contributor.employeeOjha, D.K., Tata Institute of Fundamental Research, Mumbai, India
local.issue8-
local.volume18-
dc.identifier.wos000441296300008-
local.contributor.departmentInstitute of Applied Physics, Russian Academy of Sciences, Nizhny Novgorod, Russian Federation
local.contributor.departmentLobachevsky State University of Nizhni Novgorod, Nizhny Novgorod, Russian Federation
local.contributor.departmentInstitute of Astronomy, National Central University, Taoyuan City, Taiwan
local.contributor.departmentKourovka Astronomical Observatory, Ural Federal University, Ekaterinburg, Russian Federation
local.contributor.departmentMax Planck Institute for Radio Astronomy, Bonn, Germany
local.contributor.departmentAstron. Dept., King Abdulaziz University, Jeddah, Saudi Arabia
local.contributor.departmentTata Institute of Fundamental Research, Mumbai, India
local.identifier.pure765bcbdb-1507-448e-9f84-20eca14ab69buuid
local.identifier.pure7762128-
local.description.order095-
local.identifier.eid2-s2.0-85051472390-
local.identifier.wosWOS:000441296300008-
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