The nature of the bimodal luminosity distribution of ultraluminous X-ray pulsars

Гребенев, С. А.

doi:10.1134/s1063773717050012

Cited by 20 publications

(10 citation statements)

References 26 publications

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“…"Disk winds" are thought to be observed in four NS-systems, which are Her X-1 (Kosec et al 2020;Nixon & Pringle 2020), GX 13+1 (Ueda et al 2004), IGR J17480-2446 (Miller et al 2011) and IGR J17591-2342 (Nowak et al 2019). In the first three systems, outflows are probably from the inner disk in super-Eddington accretion phase, which may be explained by the mass loss at the spherization radius because the Eddington-limited accretion is enabled (Shakura & Sunyaev 1973;Lipunova 1999;Grebenev 2017). Only in the fourth system, emission radii ranges from 1000 to 200,000 km, which is consistent with the disk wind scenario proposed in Emmering et al (1992).…”

Section: Range Of the Power Law Index Asupporting

confidence: 78%

Do the periodic activities of repeating fast radio bursts represent the spins of neutron stars?

Xu,

Li,

Yang

et al. 2021

Preprint

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Fast radio bursts (FRBs) are mysterious radio transients with millisecond durations. Recently, a periodic activity of ∼16 day and a possible periodicity of ∼159 day were detected to arise from FRB 180916.J0158+65 and FRB 121102, respectively, and the spin period of a slow-rotation magnetar was further considered to be one of possibilities to explain the periodic activities of repeating FRBs. For isolated neutron stars, the spin evolution suggests that it's difficult to reach several hours. In this work, we mainly focus on the possible maximum spin period of isolated NSs / magnetars dominated by an interaction between star's magnetic field and the disk. We find that the disk wind plays an important role in spin evolution, whose influence varies the power law index in the evolution equation of mass flow rate. For a magnetar without disk wind, the

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Section: Range Of the Power Law Index Asupporting

confidence: 78%

Do the periodic activities of repeating fast radio bursts represent the spins of neutron stars?

Xu,

Li,

Yang

et al. 2021

Preprint

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“…We will refer to such a scenario as 'classical mass loss'. Implications of this scenario to the discs around magnetized NSs were considered by Lipunov (1982) and recently by Grebenev (2017). Remarkably, because the properties of the inner disc in this model are independent of the outer boundary conditions, the size of the magnetosphere and the luminosity at higḣ M 0 converge to universal values dependent on the NS magnetic moment µ only.…”

Section: Introductionmentioning

confidence: 75%

Super-Eddington accretion discs with advection and outflows around magnetized neutron stars

Chashkina

Lipunova

Abolmasov

et al. 2019

A&A

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We present a model for a super-Eddington accretion disc around a magnetized neutron star taking into account advection of heat and the mass loss by the wind. The model is semi-analytical and predicts radial profiles of all basic physical characteristics of the accretion disc. The magnetospheric radius is found as an eigenvalue of the problem. When the inner disc is in radiation-pressuredominated regime but does not reach its local Eddington limit, advection is mild, and the radius of the magnetosphere depends weakly on the accretion rate. Once approaching the local Eddington limit, the disc becomes advection-dominated, and the scaling for the magnetospheric radius with the mass accretion rate is similar to the classical Alfvén relation. Allowing for the mass loss in a wind leads to an increase of the magnetospheric radius. Our model may be applied to a large variety of magnetized neutron stars accreting close to or above their Eddington limits: ultra-luminous X-ray pulsars, Be/X-ray binaries in outbursts, and other systems. In the context of our model we discuss the observational properties of NGC 5907 X-1, the brightest ultra-luminous pulsar known so far, and NGC 300 ULX-1 which is apparently a Be/X-ray binary experiencing a very bright super-Eddington outburst.

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“…If, alternatively, little matter fell in this zone, then we will be able to see only a double burst. The infall of matter in this zone will be considered in more detail in Grebenev (2017).…”

Section: The Origin Of the Middle Burst In A Seriesmentioning

confidence: 99%

Multiple X-ray bursts and the model of a spreading layer of accreting matter over the neutron star surface

Гребенев

Человеков

2017

Astron. Lett.

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We report the detection during the JEM-X/INTEGRAL observations of several X-ray bursters of series of close type I X-ray bursts consisting of two or three events with a recurrence time much shorter than the characteristic (at the observed mean accretion rate) time of matter accumulation needed for a thermonuclear explosion to be initiated on the neutron star surface. We show that such series of bursts are naturally explained in the model of a spreading layer of accreting matter over the neutron star surface in the case of a sufficiently high (Ṁ ∼ > 1 × 10 −9 M ⊙ yr −1 ) accretion rate (corresponding to a mean luminosity L tot ∼ > 1 × 10 37 erg s −1 ). The existence of triple bursts requires some refinement of the model -the importance of a central ring zone is shown. In the standard model of a spreading layer no infall of matter in this zone is believed to occur.

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The nature of the bimodal luminosity distribution of ultraluminous X-ray pulsars

Cited by 20 publications

References 26 publications

Do the periodic activities of repeating fast radio bursts represent the spins of neutron stars?

Do the periodic activities of repeating fast radio bursts represent the spins of neutron stars?

Super-Eddington accretion discs with advection and outflows around magnetized neutron stars

Multiple X-ray bursts and the model of a spreading layer of accreting matter over the neutron star surface

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