The 2022 super-Eddington outburst of the source SMC X-2
The 2022 super-Eddington outburst of the source SMC X-2
SMC X-2 exhibits X-ray outburst behaviour that makes it one of the most luminous X-ray sources in the Small Magellanic Cloud. In the last decade it has undergone two such massive outbursts – in 2015 and 2022. The first outburst is well reported in the literature, but the 2022 event has yet to be fully described and discussed. That is the goal of this paper. In particular, the post-peak characteristics of the two events are compared. This reveals clear similarities in decay profiles, believed to be related to different accretion mechanisms occurring at different times as the outbursts evolve. The H α emission line indicates that the Be disc undergoes complex structural variability, with evidence of warping as a result of its interaction with the neutron star. The detailed observations reported here will be important for modelling such interactions in this kind of binary systems.
astro-ph.HE, astro-ph.SR
7115-7122
Coe, M.J.
04dfb23b-1456-46a3-9242-5cee983471d5
Kennea, J.A.
8a2485ff-bd59-4dd8-b6e3-d02e86bbc344
Monageng, I.M.
c7195666-944f-4be6-93be-c4b9a5426bb4
Townsend, L.J.
b75c3b6e-ab70-4570-b388-6f24799caf74
March 2024
Coe, M.J.
04dfb23b-1456-46a3-9242-5cee983471d5
Kennea, J.A.
8a2485ff-bd59-4dd8-b6e3-d02e86bbc344
Monageng, I.M.
c7195666-944f-4be6-93be-c4b9a5426bb4
Townsend, L.J.
b75c3b6e-ab70-4570-b388-6f24799caf74
Coe, M.J., Kennea, J.A. and Monageng, I.M.
,
et al.
(2024)
The 2022 super-Eddington outburst of the source SMC X-2.
Monthly Notices of the Royal Astronomical Society, 528 (4), .
(doi:10.48550/arXiv.2402.09822).
Abstract
SMC X-2 exhibits X-ray outburst behaviour that makes it one of the most luminous X-ray sources in the Small Magellanic Cloud. In the last decade it has undergone two such massive outbursts – in 2015 and 2022. The first outburst is well reported in the literature, but the 2022 event has yet to be fully described and discussed. That is the goal of this paper. In particular, the post-peak characteristics of the two events are compared. This reveals clear similarities in decay profiles, believed to be related to different accretion mechanisms occurring at different times as the outbursts evolve. The H α emission line indicates that the Be disc undergoes complex structural variability, with evidence of warping as a result of its interaction with the neutron star. The detailed observations reported here will be important for modelling such interactions in this kind of binary systems.
Text
2402.09822v1
- Author's Original
Text
stae495
- Version of Record
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Accepted/In Press date: 14 February 2024
e-pub ahead of print date: 16 February 2024
Published date: March 2024
Keywords:
astro-ph.HE, astro-ph.SR
Identifiers
Local EPrints ID: 487979
URI: http://eprints.soton.ac.uk/id/eprint/487979
ISSN: 1365-2966
PURE UUID: 7516725e-c2ac-44f5-b64a-66b3d303273e
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Date deposited: 12 Mar 2024 17:38
Last modified: 18 Mar 2024 02:32
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Contributors
Author:
J.A. Kennea
Author:
I.M. Monageng
Author:
L.J. Townsend
Corporate Author: et al.
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