A catalogue of high-mass X-ray binaries

Liu, Q. Z.; Paradijs, J. van; Heuvel, E. P. J. van den

doi:10.1051/aas:2000288

Cited by 195 publications

(208 citation statements)

References 176 publications

(209 reference statements)

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“…Regardless of the accuracy of this association, we note that McSwain & Gies (2005) found the observed number of Be-HMXBs to be greatest between 25 and 100 Myr after star formation, relegating the vast majority of Be-HMXB activity until after the end of the simulations and the questions considered here. Be-HMXBs have been found to dominate well studied systems, such as the SMC, with transient luminosities exceeding our bright luminosity cutoff (Liu et al 2000;Antoniou et al 2009). However, current models of non-spherical winds from Be donors are not well refined, and thus the number and duration of bright Be-HMXB activity is a major source of uncertainty for our models.…”

Section: Simulation Code and Modelsmentioning

confidence: 80%

The Effect of Starburst Metallicity on Bright X-Ray Binary Formation Pathways

Linden

Kalogera

Sepinsky

et al. 2010

ApJ

180

227

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We investigate the characteristics of young (<20 Myr) and bright (L X > 1 × 10 36 erg s −1 ) high-mass X-ray binaries (HMXBs) and find the population to be strongly metallicity dependent. We separate the model populations among two distinct formation pathways: (1) systems undergoing active Roche lobe overflow (RLO) and (2) wind accretion systems with donors in the (super)giant stage, which we find to dominate the HMXB population. We find metallicity to primarily affect the number of systems which move through each formation pathway, rather than the observable parameters of systems which move through each individual pathway. We discuss the most important model parameters affecting the HMXB population at both low and high metallicities. Using these results, we show that (1) the population of ultra-luminous X-ray sources can be consistently described by very bright HMXBs which undergo stable RLO with mild super-Eddington accretion and (2) the HMXB population of the bright starburst galaxy NGC 1569 is likely dominated by one extremely metal-poor starburst cluster.

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Section: Simulation Code and Modelsmentioning

confidence: 80%

The Effect of Starburst Metallicity on Bright X-Ray Binary Formation Pathways

Linden

Kalogera

Sepinsky

et al. 2010

ApJ

180

227

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“…110 HMXB systems were known in the Milky Way before the launch of INTE-GRAL (Liu et al, 2000): 13 super-giant, 52 Be and 45 systems of unclear or other types. The serendipitous discovery by INTEGRAL of many new HMXB systems, in particular 23 likely of super-giant type, came as a surprise.…”

Section: Introductionmentioning

confidence: 99%

High-mass X-ray binaries in the Milky Way

Walter

Lutovinov

Bozzo

et al. 2015

Astron Astrophys Rev

234

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High-mass X-ray binaries are fundamental in the study of stellar evolution, nucleosynthesis, structure and evolution of galaxies and accretion processes. Hard X-rays observations by INTEGRAL and Swift have broadened significantly our understanding in particular for the super-giant systems in the Milky Way, which number has increased by almost a factor of three. INTEGRAL played a crucial role in the discovery, study and understanding of heavily obscured systems and of fast X-ray transients. Most super-giant systems can now be classified in three categories: classical/obscured, eccentric and fast transient.The classical systems feature low eccentricity and variability factor of ∼ 10 3 , mostly driven by hydrodynamic phenomena occurring on scales larger than the accretion radius. Among them, systems with short orbital periods and close to Roche-Lobe overflow or with slow winds, appear highly obscured. In eccentric systems, the variability amplitude can reach even higher factors, because of the contrast of the wind density along the orbit. Four super-giant systems, featuring fast outbursts, very short orbital periods and anomalously low accretion rates, are not yet understood.Simulations of the accretion processes on relatively large scales have progressed and reproduce parts of the observations. The combined effects of wind

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“…High-mass X-ray binaries host a compact object (a neutron star or a black hole) and a massive star (Liu et al 2000(Liu et al , 2005(Liu et al , 2006. The major subclass of high-mass X-ray binaries consists of a Be star and a compact object, and they are referred to as Be X-ray binaries (BeXRBs; e.g., Hayasaki & Okazaki 2005.…”

Section: Introductionmentioning

confidence: 99%

ON THE APPARENT LACK OF Be X-RAY BINARIES WITH BLACK HOLES

Belczyński¹,

Ziółkowski²

2009

ApJ

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In our Galaxy there are 64 Be X-ray binaries known to date. Out of these, 42 host a neutron star (NS), and for the remainder the nature of the companion is unknown. None, so far, are known to host a black hole (BH). There seems to be no apparent mechanism that would prevent formation or detection of Be stars with BHs. This disparity is referred to as a missing Be-BH X-ray binary problem. We point out that current evolutionary scenarios that lead to the formation of Be X-ray binaries predict that the ratio of binaries with NSs to the ones with BHs is rather high, F NStoBH ∼ 10-50, with the more likely formation models providing the values at the high end. The ratio is a natural outcome of (1) the stellar initial mass function that produces more NSs than BHs and (2) common envelope evolution (i.e., a major mechanism involved in the formation of interacting binaries) that naturally selects progenitors of Be X-ray binaries with NSs (binaries with comparable mass components have more likely survival probabilities) over ones with BHs (which are much more likely to be common envelope mergers). A comparison of this ratio (i.e., F NStoBH ∼ 30) with the number of confirmed Be-NS X-ray binaries (42) indicates that the expected number of Be-BH X-ray binaries is of the order of only ∼0-2. This is entirely consistent with the observed Galactic sample.

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A catalogue of high-mass X-ray binaries

Cited by 195 publications

References 176 publications

The Effect of Starburst Metallicity on Bright X-Ray Binary Formation Pathways

The Effect of Starburst Metallicity on Bright X-Ray Binary Formation Pathways

High-mass X-ray binaries in the Milky Way

ON THE APPARENT LACK OF Be X-RAY BINARIES WITH BLACK HOLES

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