Population Synthesis for Symbiotic X-ray Binaries

A. G. Kuranov; C.-H. Zhu; G.-L. Lu; K. A. Postnov; L. R. Yungelson; N. Wang

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Population Synthesis for Symbiotic X-ray Binaries

G.-L. Lu, C.-H. Zhu, K. A. Postnov, L. R. Yungelson, A. G. Kuranov, N. Wang

Solar and Stellar Astrophysics · Submitted 25 May 2012

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim We estimate the birthrate of SyXB as $\sim 4.1\times 10^{-5}$ yr$^{-1}$ to $ \sim 6.6\times 10^{-6}$ yr$^{-1}$ and their number in the Galaxy as $\sim$(100 -- 1000).

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arXiv ID1205.5696 (version 1)

Pith IDOBF4ZRTI, Pith's permanent record of this paper and its review

CitationA. G. Kuranov, C.-H. Zhu, G.-L. Lu, K. A. Postnov, L. R. Yungelson, N. Wang. "Population Synthesis for Symbiotic X-ray Binaries." arXiv:1205.5696 (2012). https://pith.science/paper/OBF4ZRTI

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The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.

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What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.85 · human participants 0.01 · controlled comparison 0.02 · randomized assignment 0.01 · states quantitative result 0.98 · compares with prior results 0.08 · mentions code or data availability 0.02.

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arXiv listing abstract v1. Results and the main claim are underlined; show every role.

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 companions, by simulation of the interaction of a magnetized neutron star (NS) with its environment and utilizing a population synthesis code. We focus mainly on the parameters that influence observational appearance of the SyXB: the donor wind velocity (vw) and the angular momentum distribution in the shell of matter settling onto NS. We estimate the birthrate of SyXB as $\sim 4.1\times 10^{-5}$ yr$^{-1}$ to $ \sim 6.6\times 10^{-6}$ yr$^{-1}$ and their number in the Galaxy as $\sim$(100 -- 1000). Assumed stellar wind velocity from cool giants is the input parameter that influences the model SyXBs population most. Among known SyXBs or candidate systems, 4U 1954+31 and IGR J16358-4724 in which NS 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 disks in 4U 1700+24, Sct X-1, IRXS J180431.1-273932 and 2XMM J174016.0-290337.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#	sentence	role	the authors' own work	states the main conclusion	strength
s0	Symbiotic X-ray binaries (SyXBs) comprise a rare class of low-mass X-ray binaries.	background 1.00	0.05	0.02	asserted 1.00
s1	We study the Galactic SyXBs, which we consider as detached binaries composed of low-mass giants and wind-fed neutron star companions, by simulation of the interaction of a magnetized neutron star (NS) with its environment and utilizing a population synthesis code.	contribution 0.68	0.93	0.05	asserted 0.99
s2	We focus mainly on the parameters that influence observational appearance of the SyXB: the donor wind velocity (vw) and the angular momentum distribution in the shell of matter settling onto NS.	contribution 0.58	0.69	0.04	asserted 0.94
s3	We estimate the birthrate of SyXB as $\sim 4.1\times 10^{-5}$ yr$^{-1}$ to $ \sim 6.6\times 10^{-6}$ yr$^{-1}$ and their number in the Galaxy as $\sim$(100 -- 1000).	result 1.00	0.93	0.43	asserted 0.95
s4	Assumed stellar wind velocity from cool giants is the input parameter that influences the model SyXBs population most.	result 0.66	0.78	0.24	asserted 0.99
s5	Among known SyXBs or candidate systems, 4U 1954+31 and IGR J16358-4724 in which NS have very long spin periods may host quasi-spherically accreting NSs.	interpretation 0.63	0.54	0.06	hedged possibility 1.00
s6	GX 1+4 has a peculiar long-term spin behaviour and it may also be a quasi-spherical wind-accreting source.	interpretation 0.67	0.42	0.04	hedged possibility 0.99
s7	We cannot identify whether there are wind-fed accretion disks in 4U 1700+24, Sct X-1, IRXS J180431.1-273932 and 2XMM J174016.0-290337.	limitation 0.72	0.80	0.03	asserted 0.67

What kind of paper the classifier reports this is: simulation study 1.00 · evidence from simulation or computation 1.00.

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full text
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Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

The paper

Original 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 companions, by simulation of the interaction of a magnetized neutron star (NS) with its environment and utilizing a population synthesis code. We focus mainly on the parameters that influence observational appearance of the SyXB: the donor wind velocity (vw) and the angular momentum distribution in the shell of matter settling onto NS. We estimate the birthrate of SyXB as $\sim 4.1\times 10^{-5}$ yr$^{-1}$ to $ \sim 6.6\times 10^{-6}$ yr$^{-1}$ and their number in the Galaxy as $\sim$(100 -- 1000). Assumed stellar wind velocity from cool giants is the input parameter that influences the model SyXBs population most. Among known SyXBs or candidate systems, 4U 1954+31 and IGR J16358-4724 in which NS 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 disks in 4U 1700+24, Sct X-1, IRXS J180431.1-273932 and 2XMM J174016.0-290337.

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References

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4 arXiv papers cite this in 5 sentences

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

Papers citing it · 3 sentences without a confident label

Contests it 1 paper

This observational distribution stands in clear conflict with the predictions of existing population-synthesis models (PSM) of WD SySts, which have consistently failed to reproduce the observed orbital period distribution [ref] .

Revisiting atmospheric Roche lobe overflow in symbiotic binaries · Introduction · contest 0.91

Cites it as background 1 paper

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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