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Modelling decretion discs in Be/X-ray binaries

Modelling decretion discs in Be/X-ray binaries
Modelling decretion discs in Be/X-ray binaries
As the largest population of high mass X-ray binaries, Be/X-ray binaries provide an excellent laboratory to investigate the extreme physics of neutron stars. It is generally accepted that Be stars possess a circumstellar disc, providing an additional source of accretion to the stellar winds present around young hot stars. Interaction between the neutron star and the disc is often the dominant accretion mechanism. A large amount of work has gone into modelling the properties of these circumstellar discs, allowing for the explanation of a number of observable phenomena. In this paper, smoothed particle hydrodynamics simulations are performed whilst varying the model parameters (orbital period, eccentricity, the mass ejection rate of the Be star and the viscosity and orientation of the disc). The relationships between the model parameters and the disc's characteristics (base gas density, the accretion rate of the neutron star and the disc's size) are presented. The observational evidence for a dependency of the size of the Be star's circumstellar disc on the orbital period (and semi-major axis) is support
ed by the simulations.
0035-8711
387-394
Brown, Rory Oliver
84b6cf9e-29e6-4390-a843-5d8f51551910
Coe, Malcolm J.
04dfb23b-1456-46a3-9242-5cee983471d5
Ho, Wynn C.G.
d78d4c52-8f92-4846-876f-e04a8f803a45
Okazaki, Atsuo T.
e6fbd972-98b2-4e4e-ab98-5afb82e799da
Brown, Rory Oliver
84b6cf9e-29e6-4390-a843-5d8f51551910
Coe, Malcolm J.
04dfb23b-1456-46a3-9242-5cee983471d5
Ho, Wynn C.G.
d78d4c52-8f92-4846-876f-e04a8f803a45
Okazaki, Atsuo T.
e6fbd972-98b2-4e4e-ab98-5afb82e799da

Brown, Rory Oliver, Coe, Malcolm J., Ho, Wynn C.G. and Okazaki, Atsuo T. (2019) Modelling decretion discs in Be/X-ray binaries. Monthly Notices of the Royal Astronomical Society, 488 (1), 387-394. (doi:10.1093/mnras/stz1757).

Record type: Article

Abstract

As the largest population of high mass X-ray binaries, Be/X-ray binaries provide an excellent laboratory to investigate the extreme physics of neutron stars. It is generally accepted that Be stars possess a circumstellar disc, providing an additional source of accretion to the stellar winds present around young hot stars. Interaction between the neutron star and the disc is often the dominant accretion mechanism. A large amount of work has gone into modelling the properties of these circumstellar discs, allowing for the explanation of a number of observable phenomena. In this paper, smoothed particle hydrodynamics simulations are performed whilst varying the model parameters (orbital period, eccentricity, the mass ejection rate of the Be star and the viscosity and orientation of the disc). The relationships between the model parameters and the disc's characteristics (base gas density, the accretion rate of the neutron star and the disc's size) are presented. The observational evidence for a dependency of the size of the Be star's circumstellar disc on the orbital period (and semi-major axis) is support
ed by the simulations.

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1906.11591 - Accepted Manuscript
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Accepted/In Press date: 24 June 2019
e-pub ahead of print date: 28 June 2019
Published date: September 2019

Identifiers

Local EPrints ID: 432385
URI: http://eprints.soton.ac.uk/id/eprint/432385
ISSN: 0035-8711
PURE UUID: 69bcffd8-58c2-4b6e-9fba-171bdf3ba838
ORCID for Malcolm J. Coe: ORCID iD orcid.org/0000-0002-0763-8547
ORCID for Wynn C.G. Ho: ORCID iD orcid.org/0000-0002-6089-6836

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Date deposited: 12 Jul 2019 16:30
Last modified: 07 Feb 2020 01:31

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