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Population synthesis for symbiotic X-ray binaries

  1. G.-L. Lü1,2,*,
  2. C.-H. Zhu1,2,
  3. K. A. Postnov3,
  4. L. R. Yungelson4,
  5. A. G. Kuranov3,
  6. N. Wang1,*

Article first published online: 10 JUL 2012

DOI: 10.1111/j.1365-2966.2012.21395.x

Issue

Monthly Notices of the Royal Astronomical Society

Monthly Notices of the Royal Astronomical Society

Volume 424, Issue 3, pages 2265–2275, 11 August 2012

Additional Information

How to Cite

Lü, G.-L., Zhu, C.-H., Postnov, K. A., Yungelson, L. R., Kuranov, A. G. and Wang, N. (2012), Population synthesis for symbiotic X-ray binaries. Monthly Notices of the Royal Astronomical Society, 424: 2265–2275. doi: 10.1111/j.1365-2966.2012.21395.x

Author Information

  1. 1

    National Astronomical Observatories/Xinjiang Observatory, The Chinese Academy of Sciences, Urumqi, China

  2. 2

    School of Physical Science and Technology, Xinjiang University, Urumqi, China

  3. 3

    Sternberg Astronomical Institute, Moscow M.V. Lomonosov State University, Moscow, Russia

  4. 4

    Institute of Astronomy of the Russian Academy of Sciences, Moscow, Russia

*E-mail: guolianglv@gmail.com (G-LL); na.wang@xao.ac.cn (NW)

Publication History

  1. Issue published online: 1 AUG 2012
  2. Article first published online: 10 JUL 2012
  3. Manuscript Accepted: 24 MAY 2012
  4. Manuscript Received: 24 MAY 2012

Funded by

  • National Natural Science Foundations of China (NSFC). Grant Numbers: 11063002, 11163005
  • Knowledge Innovation Program of the Chinese Academy of Sciences. Grant Number: KJCX2-YW-T09
  • National Basic Research Program of China. Grant Number: 973 Program 2009CB824800
  • Natural Science Foundation of Xinjiang. Grant Numbers: 2009211B01, 2010211B05
  • Doctor Foundation of Xinjiang University. Grant Number: BS100106
  • RFBR. Grant Numbers: 10-02-00951, 10-02-00231

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Keywords:

  • binaries: symbiotic;
  • stars: neutron;
  • X-rays: stars

ABSTRACT

Symbiotic X-ray binaries (SyXBs) comprise a rare class of low-mass X-ray binaries. We study the Galactic SyXBs, which we consider as detached binaries composed of low-mass giants and wind-fed neutron star (NS) companions, by simulation of the interaction of a magnetized NS with its environment and utilizing a population synthesis code. We focus mainly on the parameters that influence the observational appearance of an SyXB: the donor wind velocity (vw) and the angular momentum distribution in the shell of matter settling on to an NS. We estimate the birthrate of SyXBs as ∼4.1 × 10−5 to ∼6.6 × 10−6 yr−1 and their number in the Galaxy as ∼100–1000. The assumed stellar wind velocity from cool giants is the input parameter that influences the model SyXB population most.

Among known SyXBs or candidate systems, 4U 1954+31 and IGR J16358−4724 in which the NSs have very long spin periods may host quasi-spherically accreting NSs. GX 1+4 has a peculiar long-term spin behaviour and it may also be a quasi-spherical wind-accreting source. We cannot identify whether there are wind-fed accretion discs in 4U 1700+24, Sct X-1, IRXS J180431.1−273932 and 2XMM J174016.0−290337.

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