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Wind-accreting Symbiotic X-ray Binaries
High Energy Astrophysical Phenomena · Submitted 16 Feb 2019
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim 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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The abstract, sentence by sentence
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.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | 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. | contribution 1.00 | 0.93 | 0.13 | asserted 0.99 |
| s1 | 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. | method 0.61 | 0.79 | 0.07 | asserted 0.98 |
| s2 | 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. | result 0.97 | 0.89 | 0.37 | asserted 0.98 |
| s3 | 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. | interpretation 0.80 | 0.74 | 0.33 | asserted 0.98 |
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The paper
Original abstract
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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References
How the literature uses it
7 arXiv papers cite this in 15 sentences
Papers citing it · 7 sentences without a confident label
Uses its data or values 2 papers
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Yungelson et al. [ref] estimated that there are less than 40-50 SyXBs in the Galaxy.
Probing the Propeller Regime with Symbiotic X-ray Binaries · Introduction · 0.92
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In Fig. [ref], taken from [ref] , the number of SyXBs in the Galaxy is shown as a function of time for different formation channels (iron CC, ECSN and AIC).
The Galactic LMXB Population and the Galactic Centre Region · Symbiotic X-ray binaries · 0.83
Cites it as background 5 papers
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SyXBs are studied in many papers, see e.g. introductory part in [ref] for a brief review.
Probing the Propeller Regime with Symbiotic X-ray Binaries · Introduction · 1.00
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Generally, these are a subclass of XRB that are theorised to feature a NS accretor and a late-life giant star [ref] , although it is also theorised in rare cases that they may instead house a BH accretor [ref] .
Quiescent and Interacting Compact Remnant Binary Populations in the Space Telescope Era · Wind-fed XRBs · 0.94
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In these systems an NS is accreting from the wind of a red giant companion [ref] .
Evolution of neutron stars in wide eccentric low-mass binary systems · Introduction · 0.87
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