Journal Article

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 and J. Z. Yan

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 415, issue 4, pages 3349-3353
Published in print August 2011 | ISSN: 0035-8711
Published online August 2011 | e-ISSN: 1365-2966 | DOI: http://dx.doi.org/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

More Like This

Show all results sharing this subject:

  • Astronomy and Astrophysics

GO

Show Summary Details

Preview

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 J18483–0311; pulsars: individual: IGR J11215–5952; X-rays: binaries

Journal Article.  4600 words.  Illustrated.

Subjects: Astronomy and Astrophysics

Full text: subscription required

How to subscribe Recommend to my Librarian

Users without a subscription are not able to see the full content. Please, subscribe or login to access all content.