Be/X-ray binaries as the progenitors of the supergiant fast X-ray transients IGR J18483-0311 and IGR J11215-5952

Liu, Q. Z.; Chaty, S.; Yan, Jing-Zhi

doi:10.1111/j.1365-2966.2011.18949.x

Cited by 23 publications

(32 citation statements)

References 32 publications

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“…This source has been observed in outburst many times with INTEGRAL and Swift, and it is known to host a ∼186 s spinning NS . Due to the peculiar regularity in the occurrence of its outburst, IGR J11215-5952 is suggested to be an evolutionary link between SFXTs and BeXRBs (Liu et al, 2011). A detailed study of the supergiant star hosted in this system was presented by Lorenzo et al (2014).…”

Section: Discussionmentioning

confidence: 99%

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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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Section: Discussionmentioning

confidence: 99%

“…The supergiant with the longest orbital period, IGR J11215-5952 reaches the Be sequence. It features very regular outbursts and it has been suggested to be an evolutionary link with the Be systems (Liu et al, 2011). GX 301-2 (blue pentagon) remains persistently wind-fed by its hypergiant stellar companion, despite of its eccentric orbit.…”

Section: Corbet Diagrammentioning

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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“…These two sources are classified as "intermediate" SFXTs, and are thus thought to be the missing link between the SFXTs and classical SgXBs (due to their reduced dynamic range in the X-ray luminosity; see, e.g., Rahoui & Chaty, 2008;Giunta et al, 2009;Liu et al, 2011;Ducci et al, 2013). The cumulative luminosity distributions of these two sources have been plotted in Fig.…”

Section: Xrt Cumulative Luminosity Distributionsmentioning

confidence: 99%

Supergiant fast X-ray transients as an under-luminous class of supergiant X-ray binaries

Bozzo

Romano

Ducci

et al. 2015

Advances in Space Research

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The usage of cumulative luminosity distributions, constructed thanks to the long-term observations available through wide field hard X-ray imagers, has been recently exploited to study the averaged high energy emission (>17 keV) from Supergiant Fast X-ray Transients (SFXTs) and classical Supergiant High Mass X-ray Binaries (SgXBs). Here, we take advantage of the long term monitorings now available with Swift/XRT to construct for the first time the cumulative luminosity distributions of a number of SFXTs and the classical SgXB IGR J18027-2016 in the soft X-ray domain with a high sensitivity focusing X-ray telescope (0.3-10 keV).By complementing previous results obtained in the hard X-rays, we found that classical SgXBs are characterized by cumulative distributions with a single knee around ∼10 36 -10 37 erg s −1 , while SFXTs are found to be systematically sub-luminous and their distributions are shifted at significantly lower luminosities (a factor of ∼10-100). As the luminosity states in which these sources spend most of their time are typically below the sensitivity limit of large field of view hard X-ray imagers, we conclude that soft X-ray monitorings carried out with high sensitivity telescopes are particularly crucial to reconstruct the complete profile of the SFXT cumulative luminosity distributions.The difference between the cumulative luminosity distributions of classical SgXBs and SFXTs is interpreted in terms of accretion from a structured wind in the former sources and the presence of magnetic/centrifugal gates or a quasi-spherical settling accretion regime in the latter.

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“…Chaty 2013;Walter et al 2015, and references therein). To explain the distribution of sgHMXBs in the Corbet diagram, Liu et al (2011) argued that the majority of the systems evolved directly from OB-type main-sequence star-NS systems (i.e. without a significant accretion history since the formation of the NS), whereas a minority of the systems evolved from BeHMXBs (i.e.…”

Section: Behmxbsmentioning

confidence: 99%

Formation of Double Neutron Star Systems

Tauris

Krämer

Freire

et al. 2017

ApJ

Self Cite

642

690

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Double neutron star (DNS) systems represent extreme physical objects and the endpoint of an exotic journey of stellar evolution and binary interactions. Large numbers of DNS systems and their mergers are anticipated to be discovered using the Square-Kilometre-Array searching for radio pulsars and high-frequency gravitational wave detectors (LIGO/VIRGO), respectively. Here we discuss all key properties of DNS systems, as well as selection effects, and combine the latest observational data with new theoretical progress on various physical processes with the aim of advancing our knowledge on their formation. We examine key interactions of their progenitor systems and evaluate their accretion history during the high-mass X-ray binary stage, the common envelope phase and the subsequent Case BB mass transfer, and argue that the first-formed NSs have accreted at most ∼ 0.02 M ⊙ . We investigate DNS masses, spins and velocities, and in particular correlations between spin period, orbital period and eccentricity. Numerous Monte Carlo simulations of the second supernova (SN) events are performed to extrapolate pre-SN stellar properties and probe the explosions. All known close-orbit DNS systems are consistent with ultra-stripped exploding stars. Although their resulting NS kicks are often small, we demonstrate a large spread in kick magnitudes which may, in general, depend on the past interaction history of the exploding star and thus correlate with the NS mass. We analyze and discuss NS kick directions based on our SN simulations. Finally, we discuss the terminal evolution of close-orbit DNS systems until they merge and possibly produce a short γ-ray burst.

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Be/X-ray binaries as the progenitors of the supergiant fast X-ray transients IGR J18483-0311 and IGR J11215-5952

Cited by 23 publications

References 32 publications

High-mass X-ray binaries in the Milky Way

High-mass X-ray binaries in the Milky Way

Supergiant fast X-ray transients as an under-luminous class of supergiant X-ray binaries

Formation of Double Neutron Star Systems

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