Please use this identifier to cite or link to this item: http://elar.urfu.ru/handle/10995/131344
Title: The burst mode of accretion in massive star formation with stellar inertia
Authors: Meyer, D. M. -A.
Vorobyov, E. I.
Elbakyan, V. G.
Kraus, S.
Liu, S. -Y.
Nayakshin, S.
Sobolev, A. M.
Issue Date: 2022
Publisher: Oxford University Press
Citation: Meyer, DM-A, Vorobyov, EI, Elbakyan, VG, Kraus, S, Liu, S-Y, Nayakshin, S & Sobolev, AM 2022, 'The burst mode of accretion in massive star formation with stellar inertia', Monthly Notices of the Royal Astronomical Society, Том. 517, № 4, стр. 4795-4812. https://doi.org/10.1093/mnras/stac2956
Meyer, D. M-A., Vorobyov, E. I., Elbakyan, V. G., Kraus, S., Liu, S-Y., Nayakshin, S., & Sobolev, A. M. (2022). The burst mode of accretion in massive star formation with stellar inertia. Monthly Notices of the Royal Astronomical Society, 517(4), 4795-4812. https://doi.org/10.1093/mnras/stac2956
Abstract: The burst mode of accretion in massive star formation is a scenario linking the initial gravitational collapse of parent pre-stellar cores to the properties of their gravitationally unstable discs and of their accretion-driven bursts. In this study, we present a series of high-resolution 3D radiation-hydrodynamics numerical simulations for young massive stars formed out of collapsing 100M⊙ molecular cores, spinning with several values of the ratio of rotational-to-gravitational energies β =5-9\percent. The models include the indirect gravitational potential caused by disc asymmetries. We find that this modifies the barycentre of the disc, causing significant excursions of the central star position, which we term stellar wobbling. The stellar wobbling slows down and protracts the development of gravitational instability in the disc, reducing the number and magnitude of the accretion-driven bursts undergone by the young massive stars, whose properties are in good agreement with that of the burst monitored from the massive protostar M17 MIR. Including stellar wobbling is therefore important for accurate modelling disc structures. Synthetic alma interferometric images in the millimetre waveband show that the outcomes of efficient gravitational instability such as spiral arms and gaseous clumps can be detected for as long as the disc is old enough and has already entered the burst mode of accretion. © 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.
Keywords: METHODS: NUMERICAL
RADIATIVE TRANSFER
STARS: CIRCUMSTELLAR MATTER
MILLIMETER WAVES
STARS
BURST-MODE
GRAVITATIONAL COLLAPSE
GRAVITATIONAL INSTABILITY
MASSIVE STARS
METHOD: NUMERICAL
PRESTELLAR CORES
PROPERTY
STARS FORMATION
STARS:CIRCUMSTELLAR MATTER
STELLARS
NUMERICAL METHODS
URI: http://elar.urfu.ru/handle/10995/131344
Access: info:eu-repo/semantics/openAccess
SCOPUS ID: 85145353953
WOS ID: 000898831500006
PURE ID: 33223974
02bf87a9-bdab-4f44-aefa-2681d014a9f6
ISSN: 0035-8711
DOI: 10.1093/mnras/stac2956
metadata.dc.description.sponsorship: Horizon 2020 Framework Programme, H2020, (101003096)
Science and Technology Facilities Council, STFC, (ST/N000757/1)
University of Leicester, UoL
Ministry of Education and Science of the Russian Federation, Minobrnauka, (075-15-2020-780)
V.G. Elbakyan acknowledges support from STFC grants ST/N000757/1 to the University of Leicester. E. I. V. and A. M. S. acknowledge support of Ministry of Science and Higher Education of the Russian Federation under the grant 075-15-2020-780.
Appears in Collections:Научные публикации ученых УрФУ, проиндексированные в SCOPUS и WoS CC

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