Please use this identifier to cite or link to this item: http://hdl.handle.net/10995/103144
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dc.contributor.authorMeyer, D. M. -A.en
dc.contributor.authorVorobyov, E. I.en
dc.contributor.authorElbakyan, V. G.en
dc.contributor.authorEislöffel, J.en
dc.contributor.authorSobolev, A. M.en
dc.contributor.authorStöhr, M.en
dc.date.accessioned2021-08-31T15:07:48Z-
dc.date.available2021-08-31T15:07:48Z-
dc.date.issued2021-
dc.identifier.citationParameter study for the burst mode of accretion in massive star formation / D. M. -A. Meyer, E. I. Vorobyov, V. G. Elbakyan, et al. — DOI 10.1093/mnras/staa3528 // Monthly Notices of the Royal Astronomical Society. — 2021. — Vol. 500. — Iss. 4. — P. 4448-4468.en
dc.identifier.issn358711-
dc.identifier.otherFinal2
dc.identifier.otherAll Open Access, Green3
dc.identifier.otherhttps://www.scopus.com/inward/record.uri?eid=2-s2.0-85099693270&doi=10.1093%2fmnras%2fstaa3528&partnerID=40&md5=1ba58d3d5488663c796529d722113155
dc.identifier.otherhttp://arxiv.org/pdf/2011.05017m
dc.identifier.urihttp://hdl.handle.net/10995/103144-
dc.description.abstractIt is now a widely held view that, in their formation and early evolution, stars build up mass in bursts. The burst mode of star formation scenario proposes that the stars grow in mass via episodic accretion of fragments migrating from their gravitationally unstable circumstellar discs, and it naturally explains the existence of observed pre-main-sequence bursts from high-mass protostars. We present a parameter study of hydrodynamical models of massive young stellar objects (MYSOs) that explores the initial masses of the collapsing clouds (Mc = 60-200 Modot) and ratio of rotational-to-gravitational energies (β = 0.005-0.33). An increase in Mc and/or β produces protostellar accretion discs that are more prone to develop gravitational instability and to experience bursts. We find that all MYSOs have bursts even if their pre-stellar core is such that β ≤ 0.01. Within our assumptions, the lack of stable discs is therefore a major difference between low- and high-mass star formation mechanisms. All our disc masses and disc-to-star mass ratios Md/M⊙ > 1 scale as a power law with the stellar mass. Our results confirm that massive protostars accrete about 40, -, 60 percent of their mass in the burst mode. The distribution of time periods between two consecutive bursts is bimodal: there is a short duration (∼ 1, -, 10 yr) peak corresponding to the short, faintest bursts and a long-duration peak (at ∼ 103 104 yr) corresponding to the long, FU-Orionis-type bursts appearing in later disc evolution, i.e. around 30 kyr after disc formation. We discuss this bimodality in the context of the structure of massive protostellar jets as potential signatures of accretion burst history. © 2020 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.en
dc.format.mimetypeapplication/pdfen
dc.language.isoenen
dc.publisherOxford University Pressen
dc.rightsinfo:eu-repo/semantics/openAccessen
dc.sourceMon. Not. R. Astron. Soc.2
dc.sourceMonthly Notices of the Royal Astronomical Societyen
dc.subjectMETHODS: NUMERICALen
dc.subjectSTARS: CIRCUMSTELLAR MATTERen
dc.subjectSTARS: EVOLUTIONen
dc.subjectSTARS: FLAREen
dc.titleParameter study for the burst mode of accretion in massive star formationen
dc.typeArticleen
dc.typeinfo:eu-repo/semantics/articleen
dc.typeinfo:eu-repo/semantics/publishedVersionen
dc.identifier.doi10.1093/mnras/staa3528-
dc.identifier.scopus85099693270-
local.contributor.employeeMeyer, D.M.-A., Institut für Physik und Astronomie, Universität Potsdam, Karl-Liebknecht-Strasse 24/25, Potsdam, D-14476, Germany
local.contributor.employeeVorobyov, E.I., Department of Astrophysics, The University of Vienna, Vienna, A-1180, Austria, Institute of Astronomy, Russian Academy of Sciences, Pyatnitskaya str. 48, Moscow, 119017, Russian Federation
local.contributor.employeeElbakyan, V.G., School of Physics and Astronomy, University of Leicester, Leicester, LE1 7RH, United Kingdom
local.contributor.employeeEislöffel, J., Thüringer Landessternwarte Tautenburg, Sternwarte 5, Tautenburg, D-07778, Germany
local.contributor.employeeSobolev, A.M., Ural Federal University, 51 Lenin Str., Ekaterinburg, 620051, Russian Federation
local.contributor.employeeStöhr, M., VSC Research Center, TU Wien, Operngasse 11, Vienna, A-1040, Austria, BOKU-IT, University of Natural Resources and Life Sciences, Peter-Jordan-Strasse 82, Vienna, A-1190, Austria
local.description.firstpage4448-
local.description.lastpage4468-
local.issue4-
local.volume500-
local.contributor.departmentInstitut für Physik und Astronomie, Universität Potsdam, Karl-Liebknecht-Strasse 24/25, Potsdam, D-14476, Germany
local.contributor.departmentDepartment of Astrophysics, The University of Vienna, Vienna, A-1180, Austria
local.contributor.departmentInstitute of Astronomy, Russian Academy of Sciences, Pyatnitskaya str. 48, Moscow, 119017, Russian Federation
local.contributor.departmentSchool of Physics and Astronomy, University of Leicester, Leicester, LE1 7RH, United Kingdom
local.contributor.departmentThüringer Landessternwarte Tautenburg, Sternwarte 5, Tautenburg, D-07778, Germany
local.contributor.departmentUral Federal University, 51 Lenin Str., Ekaterinburg, 620051, Russian Federation
local.contributor.departmentVSC Research Center, TU Wien, Operngasse 11, Vienna, A-1040, Austria
local.contributor.departmentBOKU-IT, University of Natural Resources and Life Sciences, Peter-Jordan-Strasse 82, Vienna, A-1190, Austria
local.identifier.pure20515472-
local.identifier.pured7f4e63f-65b4-4bd8-8462-0bd3e7f78f6euuid
local.identifier.eid2-s2.0-85099693270-
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