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

Revnivtsev, M.; Постнов, К. А.; Куранов, А. Г.; Ritter, H. G.

doi:10.1051/0004-6361/201014726

Cited by 39 publications

(35 citation statements)

References 67 publications

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“…This relation was confirmed by observed data by Revnivtsev et al (2011). This relationship is theoretically derived from the timescale of the angular momentum loss via magnetic stellar wind (Taam 1983;Iben & Tutukov 1984).…”

Section: Roche Lobe Overflow Accretion and Luminosity-orbital Period supporting

confidence: 71%

“…1, this dependence of luminosity on the orbital period is represented by the dashed-dotted line. In the same figure, persistent LMXBs containing less-evolved donors (filled triangles) and giant donors (filled squares) are plotted (data are taken from Revnivtsev et al 2011Revnivtsev et al , 2012.…”

Section: Roche Lobe Overflow Accretion and Luminosity-orbital Period mentioning

confidence: 99%

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The nature of donors in ultraluminous X-ray binaries powered by neutron stars

Karino

2017

Monthly Notices of the Royal Astronomical Society

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In this study, we examine the properties of donor stars of the three recently discovered ultraluminous X-ray sources (ULXs) powered by rotating neutron stars. For this purpose, we constructed a theoretical relation between the X-ray luminosity (L X ) and the orbital period (P orb ) suitable for ULXs with neutron stars. By using this new L X − P orb relation, we attempt to determine the currently unknown nature of donor stars in ULXs associated with neutron stars. Especially, comparing the observed properties with the stellar evolution tracks, we suggest that the donor star in the NGC5907 ULX-1 system is a moderately massive star with 6 − 10M ⊙ , just departing from the main sequence phase. The results of our models for the other two ULX systems (M82 X-2 and NGC7793 P-13) are consistent with those in previous studies. Although there are only a few samples, observed ULX systems with neutron stars seems to involve relatively massive donors.

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Section: Roche Lobe Overflow Accretion and Luminosity-orbital Period supporting

confidence: 71%

Section: Roche Lobe Overflow Accretion and Luminosity-orbital Period mentioning

confidence: 99%

The nature of donors in ultraluminous X-ray binaries powered by neutron stars

Karino

2017

Monthly Notices of the Royal Astronomical Society

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“…Observations of other galaxies have also revealed large populations of accreting objects (Fabbiano 2006), which can be used to reveal information on the star formation history (Grimm et al 2003) and stellar content of these galaxies (Gilfanov 2004). The X-ray luminosity function of the Milky Way can be used to constrain the population and evolution of X-ray-emitting sources in the Galaxy (Grimm et al 2002), which is found to be dominated by accreting binary systems with compact object accretors (BH, NS, and WD; Revnivtsev et al 2011aRevnivtsev et al , 2011b.…”

Section: Introductionmentioning

confidence: 99%

ASWIFTSURVEY OF ACCRETION ONTO STELLAR-MASS BLACK HOLES

Reynolds

Miller

2013

ApJ

108

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We present a systemic analysis of all of the stellar-mass black hole binaries (confirmed and candidate) observed by the Swift observatory up to 2010 June. The broad Swift bandpass enables a trace of disk evolution over an unprecedented range in flux and temperature. The final data sample consists of 476 X-ray spectra containing greater than 100 counts, in the 0.6-10 keV band. This is the largest sample of high-quality CCD spectra of accreting black holes published to date. In addition, strictly simultaneous data at optical/UV wavelengths are available for 255 (54%) of these observations. The data are modeled with a combination of an accretion disk and a hard spectral component. For the hard component we consider both a simple power-law model and a thermal Comptonization model. An accretion disk is detected at greater than the 5σ confidence level in 61% of the observations. Light curves and color-color diagrams are constructed for each system. Hardness-luminosity and disk fraction-luminosity diagrams are constructed and are observed to be consistent with those typically observed by RXTE, noting the sensitivity below 2 keV provided by Swift. The observed spectra have an average luminosity of ∼1% Eddington, though we are sensitive to accretion disks down to a luminosity of 10 −3 L Edd . Thus, this is also the largest sample of such cool accretion disks studied to date. The accretion disk temperature distribution displays two peaks consistent with the classical hard and soft spectral states, with a smaller number of disks distributed between these. The distribution of inner disk radii is observed to be continuous regardless of which model is used to fit the hard continua. There is no evidence for large-scale truncation of the accretion disk in the hard state (at least for L x 10 −3 L Edd ), with all of the accretion disks having radii 40 R g . Plots of the accretion disk inner radius versus hardness ratio reveal the disk radius to be decreasing as the spectrum hardens, i.e., enters the hard state. This is in contrast to expectations from the standard disk truncation paradigm and points toward a contribution from spectral hardening. The availability of simultaneous X-ray and optical/UV data for a subset of observations facilitates a critical examination of the role of disk irradiation via a modified disk model with a variable emissivity profile (i.e., T (r) ∝ r −p ). The broadband spectra (X-ray-optical/UV) reveal irradiation of the accretion disk to be an important effect at all luminosities sampled herein, i.e., p 0.75 for luminosities 10 −3 L Edd . The accretion disk is found to dominate the UV emission irrespective of the assumed hard spectral component. Overall, we find the broadband soft-state spectra to be consistent with an irradiated accretion disk plus a corona, but we are unable to make conclusive statements regarding the nature of the hard-state accretion flow (e.g., ADAF/corona versus jet). Finally, the Swift data reveal a relation between the flux emitted by the accretion disk and that emitted b...

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“…Since there are only 12 LMXBs in the catalogue of galactic LMXBs (Liu et al, 2007), we have ignored the possible effects of LMXBs in GCs on the LMXB XLFs. The LMXB XLFs are mostly influenced by the collective emission properties of these NS-LMXBs with the break in the XLF either due to the change in the mass transfer rate in the binary systems (Postnov and Kuranov, 2005) or due to fraction of Giant donors in population of LMXBs (Revnivtsev et al, 2011). There are also an appreciable number of transient BH LMXBs, which are either in quiescence and occupy very low luminosity states or undergo outbursts for a brief period of time and occupy high luminosity end of XLFs.…”

Section: Discussionmentioning

confidence: 99%

Effects of variability of X-ray binaries on the X-ray luminosity functions of Milky Way

Islam¹,

Paul²

2016

New Astronomy

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The X-ray luminosity functions of galaxies have become a useful tool for population studies of X-ray binaries in them. The availability of long term light-curves of X-ray binaries with the All Sky X-ray Monitors opens up the possibility of constructing X-ray luminosity functions, by also including the intensity variation effects of the galactic X-ray binaries. We have constructed multiple realizations of the X-ray luminosity functions (XLFs) of Milky Way, using the long term light-curves of sources obtained in the 2-10 keV energy band with the RXTE-ASM. The observed spread seen in the value of slope of both HMXB and LMXB XLFs are due to inclusion of variable luminosities of X-ray binaries in construction of these XLFs as well as finite sample effects. XLFs constructed for galactic HMXBs in the luminosity range 10 36 − 10 39 erg/sec is described by a power-law model with a mean power-law index of -0.48 and a spread due to variability of HMXBs as 0.19. XLFs constructed for galactic LMXBs in the luminosity range 10 36 − 10 39 erg/sec has a shape of cut-off power-law with mean power-law index of -0.31 and a spread due to variability of LMXBs as 0.07. X-ray emission from a normal galaxy i.e in absence of an AGN or X-ray emitting hot gas, is dominated by collective emission from its X-ray emitting point sources (Fabbiano, 2006). With the advent of Chandra and XMM-Newton X-ray telescopes era, detailed study of X-ray emission from nearby galaxies is now possible, and has further led to the identification of X-ray binaries in them. This in turn, has helped in construction of X-ray luminosity functions (XLFs) of such galaxies. These XLFs can also act as the indicators of star formation rate, stellar mass and evolution of these galaxies (Grimm et al.

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

Cited by 39 publications

References 67 publications

The nature of donors in ultraluminous X-ray binaries powered by neutron stars

The nature of donors in ultraluminous X-ray binaries powered by neutron stars

ASWIFTSURVEY OF ACCRETION ONTO STELLAR-MASS BLACK HOLES

Effects of variability of X-ray binaries on the X-ray luminosity functions of Milky Way

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