On the evolutionary status of bright, low-mass X-ray sources

Webbink, R. F.; Rappaport, S.; Savonije, G. J.

doi:10.1086/161159

Cited by 257 publications

(204 citation statements)

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“…This is approximately correct because the total mass, which might be accreted from a late-type giant donor stars does not vary much from system to system (see e.g. Webbink et al 1983). Combining these, we obtain…”

Section: A Simple Model Of the Lmxb Luminosity Functionmentioning

confidence: 89%

“…White & Ghosh 1998;Ghosh & White 2001). Attempts to describe the LMXB LF can be found in Webbink et al (1983), but this work concentrated only on the bright end of the LF and did not consider the effects of magnetic braking on the period/luminosity distribution Table 1. The brightest persistent low mass X-ray binaries in the Galaxy with fluxes >1.4 × 10 −10 erg s −1 cm −2 measured by UHURU (Forman et al 1978 Notes.…”

Section: A Simple Model Of the Lmxb Luminosity Functionmentioning

confidence: 99%

“…It has also been noted that the most luminous LMXBs with high mass transfer rates (Ṁ > 10 −8 M /year) could harbor giant donors (see e.g. Webbink et al 1983), which may explain the difference between the low-and high-luminosity sources. The study of the LMXB LF in galaxies using population synthesis methods could potentially be quite powerful (see e.g.…”

Section: Introductionmentioning

confidence: 99%

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On the nature of the break in the X-ray luminosity function of low-mass X-ray binaries

Revnivtsev

Постнов

Куранов

et al. 2011

A&A

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We analyze a flux-limited sample of persistent and bright (with 2-10 keV fluxes exceeding 1.4 × 10 −10 erg s −1 cm −2 ) low-mass X-ray binaries (LMXBs) in our Galaxy. It is demonstrated that the majority of binary systems with X-ray luminosities below log L(erg/s) ∼ 37.3 have unevolved secondary companions (except for those with white dwarf donors), while systems with higher X-ray luminosity harbor predominantly giant donors. Mass transfer in binary systems with giants significantly shortens their lifetime thus steepening the X-ray luminosity function of LMXBs at high luminosity. We argue that this is why the LMXB luminosity function constructed from observations of sources in our and distant galaxies demonstrates a break at log L(erg/s) ∼ 37.3.

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Section: A Simple Model Of the Lmxb Luminosity Functionmentioning

confidence: 89%

Section: A Simple Model Of the Lmxb Luminosity Functionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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On the nature of the break in the X-ray luminosity function of low-mass X-ray binaries

Revnivtsev

Постнов

Куранов

et al. 2011

A&A

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“…On the other hand, Muñoz-Darias et al (2008) calculated the theoretical mass transfer rate in GX 339-4 using the model of King (1993) (who used the evolutionary calculations of Webbink, Rappaport & Savonije 1983) as −Ṁ 2 < 8 × 10 −10 M ⊙ yr −1 , i.e., 16 times less than the observational estimate of Coriat et al (2012). Clearly, that theoretical maximum is strongly violated by the observational data.…”

Section: The Parameters Of Gx 339-4mentioning

confidence: 99%

Spectral analysis of theXMM–Newtondata of GX 339–4 in the low/hard state: disc truncation and reflection

Basak¹,

Zdziarski²

2016

Mon. Not. R. Astron. Soc.

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We analyse all available observations of GX 339-4 by XMM-Newton in the hard spectral state. We jointly fit the spectral data by Comptonization and the currently best reflection code, relxill. We consider in detail a contribution from a standard blackbody accretion disc, testing whether its inner radius can be set equal to that of the reflector. However, this leads to an unphysical behaviour of the disc truncation radius, implying the soft X-ray component is not a standard blackbody disc. This appears to be due to irradiation by the hard X-rays, which strongly dominate the total emission. We consider a large array of models, testing, e.g., the effects of the chosen energy range, of adding unblurred reflection, and assuming a lamppost geometry. We find the effects of relativistic broadening to be relatively weak in all cases. In the coronal models, we find the inner radius to be large. In the lamppost model, the inner radius is unconstrained, but when fixed to the innermost stable orbit, the height of the source is large, which also implies a weak relativistic broadening. In the former models, the inner radius correlates with the X-ray hardness ratio, which is consistent with the presence of a truncated disc turning into a complete disc in the soft state. We also find the degree of the disc ionization to anti-correlate with the hardness, leading to strong spectral broadening due to scattering of reflected photons in the reflector in the softest studied states.

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“…In that limit, and using the measured Chandra position of sources at such locations, such a wide (10 day) binary would be detectable at B or V in a observation with the Advanced Camera for Sur- If the disk is thermally stable and transfers matter to the NS at the supplied rate, there is nearly a one-to-one relation between and the X-ray luminosity (see Fig. 1) that would allow P i the orbital period distribution to be inferred from the luminosity distribution (Webbink, Rappaport, & Savonije 1983). However, this argument fails because these wide binaries are almost always transient accretors.…”

Section: Binary Evolution With Red Giant Donorsmentioning

confidence: 99%

Transient X-Ray Binaries in Elliptical Galaxies

Piro

Bildsten

2002

The Astrophysical Journal

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Chandra observations of elliptical galaxies have revealed large numbers of low-mass X-ray binaries (LMXBs) accreting at rates greater than 10 Ϫ9 M , yr . One scenario that generates this from an old stellar population Ϫ1Ṁis nuclear-driven mass transfer onto a neutron star or black hole from a Roche lobe-filling red giant. However, in our Galaxy, most of these systems accrete sporadically as transients because of a thermal instability in the accretion disk. Using the common criterion for disk instability (including irradiation), we find that this mode of mass transfer leads to transient accretion for at least 75% of the binary's life. Repeated Chandra observations of elliptical galaxies should reveal this population. The recurrence times might be very long (∼100-10,000 yr depending on the orbital period at the onset of mass transfer), and outbursts might last for 1-100 yr. Mass transferring binaries can also be formed in old populations via interactions in dense stellar environments, such as globular clusters. These tend to have shorter orbital periods and are more likely stable accretors, making them apparently a large fraction of an elliptical galaxy's LMXB population.

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On the evolutionary status of bright, low-mass X-ray sources

Cited by 257 publications

References 0 publications

On the nature of the break in the X-ray luminosity function of low-mass X-ray binaries

On the nature of the break in the X-ray luminosity function of low-mass X-ray binaries

Spectral analysis of theXMM–Newtondata of GX 339–4 in the low/hard state: disc truncation and reflection

Transient X-Ray Binaries in Elliptical Galaxies

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