Discovery of a short orbital period in the Supergiant Fast X-ray Transient IGR J16479–4514

Jain, Chetana; Paul, Biswajit; Dutta, A.

doi:10.1111/j.1745-3933.2009.00668.x

Cited by 55 publications

(61 citation statements)

References 49 publications

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“…Some authors have suggested that the eclipse by the SG star causes the X-ray dark phase in this system (Bozzo et al 2008b). Since this system shows marginal properties between the classical OB-type HMXB and an SFXT, it could be a prototype system that bridges new and classical understandings of HMXBs (Sguera et al 2008;Jain et al 2009). Further observations and discussions on this source are strongly required.…”

Section: Discussionmentioning

confidence: 99%

“…In the list of observed SFXTs (Table 1), IGR J16479-4514 has an extremely short orbital period, P orb = 3.2 d (Jain et al 2009). Although it is suggested that this system has a large eccentricity, such a system with short orbital period likely becomes a persistent source or contact binary, according to our result (see Fig.…”

Section: Discussionmentioning

confidence: 99%

“…At least for a few systems, the clumpy wind model seems to reconstruct these observed properties very well (for example, IGR J17544-2619, see in 't Zand 2005; Clark et al 2009). On the other hand, however, there are serious difficulties for few systems (for example, IGR J11215-5952 and IGR J16479-4514) to explain the observed parameters under the clumpy wind assumption Romano et al 2009b;Bozzo et al 2008b;Romano et al 2008;Jain et al 2009). Hence, it is considered that the clumpy wind model has a certain limit of application.…”

Section: Modelmentioning

confidence: 99%

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Orbital parameters of supergiant fast X-ray transients

Karino

2010

A&A

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Context. Supergiant fast X-ray transient (SFXT) is a new class of the high-mass X-ray binary that shows short X-ray flares. The physical mechanism of SFXT short flares is still open for discussion. The accretion process of dense clumps in stellar wind onto neutron star (NS) has been proposed as the origin of such short flares. Aims. In order to examine the applicability of the clumpy wind scenario, we focus on the accretion mode that depends on orbital parameters. Our goal is to impose restrictions on the orbital parameters of SFXT. Methods. Assuming a simple analytic model of clumpy wind, we investigate the condition where the size of accretion cylinder overcomes the clump size. Results. The allowed parameter region for SFXT is restricted in a relatively narrow window in P orb − e diagram. Conclusions. Binary systems with large eccentricities (e > ∼ 0.4) and moderate orbital periods (P orb ∼ 10 d) are prone to show periodic X-ray outbursts, which are characteristic for SFXT. We confirm that systems with a long orbital period of more than 100 days cannot produce bright X-ray flares in the simple clumpy wind scenario.

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Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Section: Modelmentioning

confidence: 99%

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Orbital parameters of supergiant fast X-ray transients

Karino

2010

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“…Therefore, this class of systems can be an accretor with retrograde accretion. In addition, IGR J16479-4514, with P s = 2.14 s (http://hera.ph1.uni-koeln.de/~heintzma/ Integral/SFXT.htm) and P orb = 3.3 days (Jain et al 2009), also present a somewhat larger corotation radius. Therefore, it can also behave like an retrograde accretor.…”

Section: Application To Sfxtsmentioning

confidence: 99%

“…de/~heintzma/Integral/SFXT.htm, P orb = 18 days, Jain et al 2009; for IGR J17544-2619, P s = 71.49 s, Drave et al 2012, P orb = 4.9 days, Clark et al 2010. From the expressions of r mag and r cor (see Eqs.…”

Section: Application To Sfxtsmentioning

confidence: 99%

Retrograde wind accretion – an alternative mechanism for long spin period of SFXTs

Wang

Chang

2012

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A new class of high-mass X-ray binaries (HMXBs) -supergiant fast X-ray transients (SFXTs) -are discovered by INTEGRAL, which are associated with OB supergiants and present long spin periods. Observational evidence indicates that some accreting neutron stars in HMXBs display accretion reversals. It has been suggested that the inverted torque can lead to a very slow rotator. According to three characteristic radii in wind-fed accretion, we developed a retrograde accretion scenario and divided the accretion phase into three regimes, to interpret the formation of the long spin period of SFXTs. The accretion regime in some SFXT systems can be determined by their spin and orbital periods.

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Towards a Unified View of Inhomogeneous Stellar Winds in Isolated Supergiant Stars and Supergiant High Mass X-Ray Binaries

et al. 2017

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Massive stars, at least ∼ 10 times more massive than the Sun, have two key properties that make them the main drivers of evolution of star clusters, galaxies, and the Universe as a whole. On the one hand, the outer layers of massive stars are so hot that they produce most of the ionizing ultraviolet radiation of galaxies; in fact, the first massive stars helped to re-ionize the Universe after its Dark Ages. Another important property of massive stars are the strong stellar winds and outflows they produce. This mass loss, and finally the explosion of a massive star as a supernova or a gamma-ray burst, provide a significant input of mechanical and radiative energy into the interstellar space. These two properties together make massive stars one of the most important cosmic engines: they trigger the star formation and enrich the interstellar medium with heavy elements, that ultimately leads to formation of Earth-like rocky planets and the development of complex life. The study of massive star winds is thus a truly multidisciplinary field and has a wide impact on different areas of astronomy.In recent years observational and theoretical evidences have been growing that these winds are not smooth and homogeneous as previously assumed, but rather populated by dense "clumps". The presence of these structures dramatically affects the mass loss rates derived from the study of stellar winds. Clump properties in isolated stars are nowadays inferred mostly through indirect methods (i.e., spectroscopic observations of line profiles in various wavelength regimes, and their analysis based on tailored, inhomogeneous wind models). The limited characterization of the clump physical properties (mass, size) obtained so far have led to large uncertainties in the mass loss rates from massive stars. Such uncertainties limit our understanding of the role of massive star winds in galactic and cosmic evolution.Supergiant high mass X-ray binaries (SgXBs) are among the brightest X-ray sources in the sky. A large number of them consist of a neutron star accreting from the wind of a massive companion and producing a powerful X-ray source. The characteristics of the stellar wind together with the complex interactions between the compact object and the donor star determine the observed X-ray output from all these systems. Consequently, the use of SgXBs for studies of massive stars is only possible when the physics of the stellar winds, the compact objects, and accretion mechanisms are combined together and confronted with observations. This detailed review summarises the current knowledge on the theory and observations of winds from massive stars, as well as on observations and accretion processes in wind-fed high mass X-ray binaries. The aim is to combine in the near future all available theoretical Unified view of of inhomogeneous stellar winds in supergiant stars and HXMB 3 diagnostics and observational measurements to achieve a unified picture of massive star winds in isolated objects and in binary systems.

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Discovery of a short orbital period in the Supergiant Fast X-ray Transient IGR J16479–4514

Cited by 55 publications

References 49 publications

Orbital parameters of supergiant fast X-ray transients

Orbital parameters of supergiant fast X-ray transients

Retrograde wind accretion – an alternative mechanism for long spin period of SFXTs

Towards a Unified View of Inhomogeneous Stellar Winds in Isolated Supergiant Stars and Supergiant High Mass X-Ray Binaries

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