Wind-accreting Symbiotic X-ray Binaries. (arXiv:1902.06060v1 [astro-ph.HE])

Wind-accreting Symbiotic X-ray Binaries. (arXiv:1902.06060v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Yungelson_L/0/1/0/all/0/1">Lev Yungelson</a> (INASAN RAS), <a href="http://arxiv.org/find/astro-ph/1/au:+Kuranov_A/0/1/0/all/0/1">Alexandre Kuranov</a> (SAI MSU), <a href="http://arxiv.org/find/astro-ph/1/au:+Postnov_K/0/1/0/all/0/1">Konstantin Postnov</a> (SAI MSU)

We present a new model of the population of symbiotic X-ray binaries (SyXBs)
that takes into account non-stationary character of quasi-spherical sub-sonic
accretion of the red giant’s stellar wind onto slowly rotating neutron stars.
Updates of the earlier models are given, which include more strict criteria of
slow NS rotation for plasma entry into the NS magnetosphere via Rayleigh-Taylor
instability, as well as more strict conditions for settling accretion for slow
stellar winds, with an account of variations in the specific angular momentum
of captured stellar wind in eccentric binaries. These modifications enabled a
more adequate description of the distributions of observed systems over binary
orbital periods, NS spin periods and their X-ray luminosity in the $sim
10^{32}-10^{36}$~erg s$^{-1}$ range and brought their model Galactic number
into reasonable agreement with the observed one. Reconciliation of the model
and observed orbital periods of SyXBs requires a low efficiency of matter
expulsion from common envelopes during the evolution that results in the
formation of NS-components of symbiotic X-ray systems.

We present a new model of the population of symbiotic X-ray binaries (SyXBs)
that takes into account non-stationary character of quasi-spherical sub-sonic
accretion of the red giant’s stellar wind onto slowly rotating neutron stars.
Updates of the earlier models are given, which include more strict criteria of
slow NS rotation for plasma entry into the NS magnetosphere via Rayleigh-Taylor
instability, as well as more strict conditions for settling accretion for slow
stellar winds, with an account of variations in the specific angular momentum
of captured stellar wind in eccentric binaries. These modifications enabled a
more adequate description of the distributions of observed systems over binary
orbital periods, NS spin periods and their X-ray luminosity in the $sim
10^{32}-10^{36}$~erg s$^{-1}$ range and brought their model Galactic number
into reasonable agreement with the observed one. Reconciliation of the model
and observed orbital periods of SyXBs requires a low efficiency of matter
expulsion from common envelopes during the evolution that results in the
formation of NS-components of symbiotic X-ray systems.

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