Probing the Propeller Regime with Symbiotic X-ray Binaries

M.D. Afonina (SAI MSU); S.B. Popov (ICTP)

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Probing the Propeller Regime with Symbiotic X-ray Binaries

M.D. Afonina (SAI MSU), S.B. Popov (ICTP)

High Energy Astrophysical Phenomena · Submitted 26 Apr 2024

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

The authors' main claim Only in the case of a relatively slow propeller model proposed by Davies and Pringle (1981), the duration of the propeller is long enough to provide a significant probability to observe the system at this stage.

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Compiled by classifier-1.13.0 via TypeSafe API, question bank abstract-p1-20260923, 2026-09-23: 1 request, 4,897 input tokens.

What the abstract itself states, as probabilities: claims first 0.04 · states limitation 0.73 · human participants 0.01 · controlled comparison 0.07 · randomized assignment 0.01 · states quantitative result 0.08 · compares with prior results 0.64 · mentions code or data availability 0.02.

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At the moment, there are two neutron star X-ray binaries with massive red supergiants as donors. De et al. (2023) proposed that the system SWIFT J0850.8-4219 contains a neutron star at the propeller stage. We study this possibility by applying various models of propeller spin-down. We demonstrate that the duration of the propeller stage is very sensitive to the regime of rotational losses. Only in the case of a relatively slow propeller model proposed by Davies and Pringle (1981), the duration of the propeller is long enough to provide a significant probability to observe the system at this stage. Future determination of the system parameters (orbital and spin periods, magnetic field of the compact object, etc.) will allow putting strong constraints on the propeller behavior.

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	At the moment, there are two neutron star X-ray binaries with massive red supergiants as donors.	background 1.00	0.09	0.02	asserted 1.00
s1	De et al. (2023) proposed that the system SWIFT J0850.8-4219 contains a neutron star at the propeller stage.	background 0.99	0.03	0.04	hedged possibility 0.84
s2	We study this possibility by applying various models of propeller spin-down.	method 0.78	0.84	0.03	asserted 0.87
s3	We demonstrate that the duration of the propeller stage is very sensitive to the regime of rotational losses.	result 0.98	0.84	0.19	asserted 1.00
s4	Only in the case of a relatively slow propeller model proposed by Davies and Pringle (1981), the duration of the propeller is long enough to provide a significant probability to observe the system at this stage.	result 0.91	0.73	0.80	asserted 0.97
s5	Future determination of the system parameters (orbital and spin periods, magnetic field of the compact object, etc.) will allow putting strong constraints on the propeller behavior.	future work 1.00	0.05	0.09	hedged possibility 0.85

What kind of paper the classifier reports this is: theoretical result 0.78 · evidence from argument 0.49.

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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

At the moment, there are two neutron star X-ray binaries with massive red supergiants as donors. De et al. (2023) proposed that the system SWIFT J0850.8-4219 contains a neutron star at the propeller stage. We study this possibility by applying various models of propeller spin-down. We demonstrate that the duration of the propeller stage is very sensitive to the regime of rotational losses. Only in the case of a relatively slow propeller model proposed by Davies and Pringle (1981), the duration of the propeller is long enough to provide a significant probability to observe the system at this stage. Future determination of the system parameters (orbital and spin periods, magnetic field of the compact object, etc.) will allow putting strong constraints on the propeller behavior.

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2 arXiv papers cite this in 3 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 · 1 sentence without a confident label

Builds on it 1 paper

In the first paper [ref] , we applied various propeller models to analyse magneto-rotational evolution of NSs in symbiotic X-ray binaries.

Evolution of neutron stars in wide eccentric low-mass binary systems · Introduction · 0.88

Uses its data or values 1 paper

The NS can both spin up and spin down, so the angular momentum consists of two terms [equation] The spin-down torque is [equation] where coefficient $k_t=0.4$ [ref] .

Evolution of neutron stars in wide eccentric low-mass binary systems · Magneto-rotational evolution of a neutron star · 0.83

What it cites · 37 sentences without a confident label

Uses the method or tool of 3 papers

In [ref] the authors use the following equation:

Infrared spectroscopy of SWIFT J0850.8-4219: Identification of the second red supergiant X-ray binary in the Milky Way · Stellar wind · 0.85
To reach this goal, we utilize PARSEC evolutionary tracks [ref] .

PARSEC evolutionary tracks of massive stars up to $350 M_\odot$ at metallicities 0.0001$\leq Z \leq$0.04 · Stellar wind · 0.93
With the mass, radius, and temperature known, we calculate the wind velocity following the prescription from [ref] .

New theoretical Mass-loss rates of O and B Stars · Stellar wind · 1.00

Uses data or values from 3 papers

According to [ref] this parameter is $ζ∼10^-2$.

Infrared spectroscopy of SWIFT J0850.8-4219: Identification of the second red supergiant X-ray binary in the Milky Way · Luminosity at the propeller stage · 0.98
Yungelson et al. [ref] estimated that there are less than 40-50 SyXBs in the Galaxy.

Wind-accreting Symbiotic X-ray Binaries · Introduction · 0.92
The dependence of the ratio $v_w/v_∞$ for K4 type RSGs is shown in [ref] .

Chromospheres and Winds of Red Supergiants: An Empirical Look at Outer Atmospheric Structure · Stellar wind · 0.91

Cites as background 10 papers

We distinguish four main evolutionary stages: ejector, propeller, accretor, and georotator (see [ref] ).

Spin evolution of neutron stars · Spin evolution of NSs · 0.94
This accretion regime has been proposed in [ref] and later considered in detail in the series of papers [ref] .

Settling accretion onto slowly rotating X-ray pulsars · The possibility of settling accretion in SWIFT J0850.8-4219 · 0.84
This accretion regime has been proposed in [ref] and later considered in detail in the series of papers [ref] .

Theory of wind accretion · The possibility of settling accretion in SWIFT J0850.8-4219 · 0.84

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