Be/X-ray binaries

Reig, P.

doi:10.1007/s10509-010-0575-8

Cited by 545 publications

(538 citation statements)

References 139 publications

(148 reference statements)

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“…The optical counterpart of the system is a B0 V-IIIe star LS 1698 at the distance of ∼ 5 kpc (Motch et al, 1997). Timing analysis of the RXTE data revealed pulsations in the source flux with a period of P ≃ 860 s and it was suggested that the system belongs to the subclass of persistent Be/X-ray systems with slowly rotating neutron stars (Reig, 2011). A possible association of 4U 1036-56 with the unidentified transient gamma-ray source AGL J1037-5708 was discussed by Li et al (2012a).…”

Section: Discussionmentioning

confidence: 99%

“…Similarly other such systems its spectrum is characterized by a presence of the soft thermal component with the temperature of kT ∼ 1 keV and the power-low tail at higher energies (La Palombara and Mereghetti, 2006). The source is the X-ray pulsar with a quite long pulse period P spin ≃ 25 min, which was discovered by the EXOSAT observatory and erroneously related to the nearby source 4U 0142+614 (White et al, 1987;Reig, 2011). The system is located in the open cluster NGC 663 at a distance of 2.5 kpc (Tapia et al, 1991).…”

Section: Discussionmentioning

confidence: 99%

“…Using these data Apparao et al (1980) found pulsations from the source with the period P spin ≃ 17.64 sec. Based on the accurate measurements of the source position with the Einstein observatory and following optical observations it was shown that an optical counterpart in the system is a Be star (Grindlay et al, 1984) with a spectral type B1Ve (Reig, 2011). Long observations performed with the BATSE instrument on board the Comptom-GRO observatory in 1994 allowed to determine orbital parameters of the system and showed that a neutron star is orbiting in a highly eccentric orbit (eccentricity e = 0.446) with the period P orb = 42.12 days (Finger et al, 1996a).…”

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%

Section: Discussionmentioning

confidence: 99%

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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“…Binder et al (2016) propose the interesting hypothesis that the initial outburst of SN2010da marked the onset of the HMXB phase based on the recurring X-ray bursts and the presumed quiescence of the progenitor, where L X <(3-9)×10 36 erg s −1 at fourepochs. HMXBs are accretion-powered binary systems with an NS or black hole orbiting an O-or B-type companion and are subdivided into two subclasses depending on the evolutionary status of the optical companion (Liu et al 2005;Reig 2011). The most common types of HMXBs (∼60%; Liu et al 2006) are known as Be/X-ray binaries (BeXBs) and host a rapidly rotating, non-supergiant B-type star with low-ionization emission lines attributed to an equatorial "excretion" disk of material ejected from the star.…”

Section: Introductionmentioning

confidence: 99%

RISING FROM THE ASHES: MID-INFRARED RE-BRIGHTENING OF THE IMPOSTOR SN 2010da IN NGC 300

Lau

Kasliwal

Bond

et al. 2016

ApJ

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We present multi-epoch mid-infrared (IR) photometry and the optical discovery observations of the "impostor" supernova (SN) 2010da in NGC300 using new and archival Spitzer Space Telescope images and ground-based observatories. The mid-infrared counterpart of SN2010da was detected as Spitzer Infrared Intensive Transient Survey (SPIRITS)14bme in the SPIRITS, an ongoing systematic search for IR transients. Before erupting on 2010 May 24, the SN2010da progenitor exhibited a constant mid-IR flux at 3.6 and only a slight ∼10% decrease at 4.5 μm between 2003 November and 2007 December. A sharp increase in the 3.6 μm flux followed by a rapid decrease measured ∼150 days before and ∼80 days after the initial outburst, respectively, reveal a mid-IR counterpart to the coincident optical and high luminosity X-ray outbursts. At late times, after the outburst (∼2000 days), the 3.6 and 4.5 μm emission increased to over a factor of twotimes the progenitor flux and is currently observed (as of 2016 Feb) to be fading, but still above the progenitor flux. We attribute the re-brightening mid-IR emission to continued dust production and increasing luminosity of the surviving system associated with SN2010da. We analyze the evolution of the dust temperature (T d ∼700-1000 K), mass (M d ∼0.5-3.8×10 −7 M e ), luminosity (L IR ∼1.3-3.5×10 4 L e ), and the equilibrium temperature radius (R eq ∼6.4-12.2 au) in order to resolve the nature of SN2010da. We address the leading interpretation of SN2010da as an eruption from a luminous blue variable high-mass X-ray binary (HMXB) system. We propose that SN2010da is instead a supergiant (sg)B[e]-HMXB based on similar luminosities and dust masses exhibited by two other known sgB[e]-HMXB systems. Additionally, the SN2010da progenitor occupies a similar region on a mid-IR color-magnitude diagram (CMD) with known sgB[e] stars in the Large Magellanic Cloud. The lower limit estimated for the orbital eccentricity of the sgB[e]-HMXB (e>0.82) from X-ray luminosity measurements is high compared to known sgHMXBs and supports the claim that SN2010da may be associated with a newly formed HMXB system.

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“…The majority of these HMXBs are Be/X-ray binaries (BeX) in which a neutron star orbits around a massive (≥ 10 M ) and rapidly rotating (≥ 80% of break-up velocity) Be star [1]. The orbit of the system is generally very wide (P ∼ 20 -200 d) and eccentric (0.1 < e < 0.9).…”

Section: Introductionmentioning

confidence: 99%

SALT observations of the Be/X-ray binary A0538-66

Rajoelimanana¹,

Meintjes²,

Charles³

et al. 2016

Proceedings of SALT Science Conference 2015 — PoS(SSC2015)

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The Be X-ray transient, A0538-66, is the most extreme LMC/SMC member of this class, exhibiting optical (and sometimes X-ray) outbursts with a period of 16.6d. More remarkably, long-term (MACHO) optical photometry revealed a large amplitude (∼0.5mag) 421d activity cycle which appears to control the appearance of the recurrent orbital outbursts/flares, as they are only seen during the minimum of the 421d cycle. The nature of the physical link between these features is very poorly understood, but is likely related to properties of the Be star's equatorial disc. We will present our recent results on the long-term spectroscopic observations of this LMC BeX system using both broad-band (wide wavelength coverage) as well as high resolution optical spectra obtained from the Southern African Large Telescope (SALT). These observations enable us to probe both the evolution of the Be star envelope and the details of its interaction with the neutron star in its presumed highly eccentric (e ∼ 0.7) orbit. The high resolution spectra also allows us to derive its rotational velocity and spectral classification.

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Be/X-ray binaries

Cited by 545 publications

References 139 publications

High-mass X-ray binaries in the Milky Way

High-mass X-ray binaries in the Milky Way

RISING FROM THE ASHES: MID-INFRARED RE-BRIGHTENING OF THE IMPOSTOR SN 2010da IN NGC 300

SALT observations of the Be/X-ray binary A0538-66

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