Be/X-ray binaries as the progenitors of the supergiant fast X-ray transients IGR J18483-0311 and IGR J11215-5952

Q. Z. Liu; S. Chaty; J. Z. Yan

doi:10.1111/j.1365-2966.2011.18949.x

Be/X-ray binaries as the progenitors of the supergiant fast X-ray transients IGR J18483-0311 and IGR J11215-5952

Q. Z. Liu, S. Chaty, J. Z. Yan

Research output: Contribution to journal › Article › peer-review

Abstract

The relation between the spin period (P_s) and the orbital period (P_o) in high-mass X-ray binaries is investigated. Be/X-ray binaries and SG/X-ray binaries occupy different areas in the Corbet diagram. The supergiant fast X-ray transients, IGR J18483-0311 and IGR J11215-5952, however, fall into the area occupied by Be/X-ray binaries. After excluding the other evolution scenarios, we find that the positions of the two supergiant fast X-ray transients in the diagram can be interpreted by being the descendants of O-emission X-ray binaries, i.e. the supergiant stars in these systems formed from O-type emission line stars instead of normal main-sequence stars. Therefore, we suggest that there are two types of SG/X-ray binaries: the first one is directly evolved from OB-type main-sequence star and neutron star systems without accretion history, and the other evolved from Be/X-ray binaries with accretion history.

Original language	English
Pages (from-to)	3349-3353
Number of pages	5
Journal	Monthly Notices of the Royal Astronomical Society
Volume	415
Issue number	4
DOIs	https://doi.org/10.1111/j.1365-2966.2011.18949.x
Publication status	Published - 1 Jan 2011
Externally published	Yes

Keywords

Binaries: close
Pulsars: individual: IGR J11215-5952
Pulsars: individual: IGR J18483-0311
X-rays: binaries

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10.1111/j.1365-2966.2011.18949.x

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title = "Be/X-ray binaries as the progenitors of the supergiant fast X-ray transients IGR J18483-0311 and IGR J11215-5952",

abstract = "The relation between the spin period (Ps) and the orbital period (Po) in high-mass X-ray binaries is investigated. Be/X-ray binaries and SG/X-ray binaries occupy different areas in the Corbet diagram. The supergiant fast X-ray transients, IGR J18483-0311 and IGR J11215-5952, however, fall into the area occupied by Be/X-ray binaries. After excluding the other evolution scenarios, we find that the positions of the two supergiant fast X-ray transients in the diagram can be interpreted by being the descendants of O-emission X-ray binaries, i.e. the supergiant stars in these systems formed from O-type emission line stars instead of normal main-sequence stars. Therefore, we suggest that there are two types of SG/X-ray binaries: the first one is directly evolved from OB-type main-sequence star and neutron star systems without accretion history, and the other evolved from Be/X-ray binaries with accretion history.",

keywords = "Binaries: close, Pulsars: individual: IGR J11215-5952, Pulsars: individual: IGR J18483-0311, X-rays: binaries",

author = "Liu, \{Q. Z.\} and S. Chaty and Yan, \{J. Z.\}",

year = "2011",

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doi = "10.1111/j.1365-2966.2011.18949.x",

language = "English",

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T1 - Be/X-ray binaries as the progenitors of the supergiant fast X-ray transients IGR J18483-0311 and IGR J11215-5952

AU - Liu, Q. Z.

AU - Chaty, S.

AU - Yan, J. Z.

PY - 2011/1/1

Y1 - 2011/1/1

N2 - The relation between the spin period (Ps) and the orbital period (Po) in high-mass X-ray binaries is investigated. Be/X-ray binaries and SG/X-ray binaries occupy different areas in the Corbet diagram. The supergiant fast X-ray transients, IGR J18483-0311 and IGR J11215-5952, however, fall into the area occupied by Be/X-ray binaries. After excluding the other evolution scenarios, we find that the positions of the two supergiant fast X-ray transients in the diagram can be interpreted by being the descendants of O-emission X-ray binaries, i.e. the supergiant stars in these systems formed from O-type emission line stars instead of normal main-sequence stars. Therefore, we suggest that there are two types of SG/X-ray binaries: the first one is directly evolved from OB-type main-sequence star and neutron star systems without accretion history, and the other evolved from Be/X-ray binaries with accretion history.

AB - The relation between the spin period (Ps) and the orbital period (Po) in high-mass X-ray binaries is investigated. Be/X-ray binaries and SG/X-ray binaries occupy different areas in the Corbet diagram. The supergiant fast X-ray transients, IGR J18483-0311 and IGR J11215-5952, however, fall into the area occupied by Be/X-ray binaries. After excluding the other evolution scenarios, we find that the positions of the two supergiant fast X-ray transients in the diagram can be interpreted by being the descendants of O-emission X-ray binaries, i.e. the supergiant stars in these systems formed from O-type emission line stars instead of normal main-sequence stars. Therefore, we suggest that there are two types of SG/X-ray binaries: the first one is directly evolved from OB-type main-sequence star and neutron star systems without accretion history, and the other evolved from Be/X-ray binaries with accretion history.

KW - Binaries: close

KW - Pulsars: individual: IGR J11215-5952

KW - Pulsars: individual: IGR J18483-0311

KW - X-rays: binaries

U2 - 10.1111/j.1365-2966.2011.18949.x

DO - 10.1111/j.1365-2966.2011.18949.x

M3 - Article

AN - SCOPUS:80051814862

SN - 0035-8711

VL - 415

SP - 3349

EP - 3353

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 4

ER -

Be/X-ray binaries as the progenitors of the supergiant fast X-ray transients IGR J18483-0311 and IGR J11215-5952

Abstract

Keywords

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