The optical counterpart to IGR J06074+2205: a Be/X-ray binary showing disc loss and<i>V/R</i>variability

Reig, P.; Zezas, A.; Gkouvelis, Leonardos

doi:10.1051/0004-6361/201014788

Cited by 28 publications

(18 citation statements)

References 39 publications

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“…A number of studies were dedicated to the search of the optical counterpart of this source (Halpern and Tyagi, 2005;Tomsick et al, 2006b;Masetti et al, 2006a;Reig and Zezas, 2009;Reig et al, 2010). Finally Reig et al (2010) identified it with a relatively bright (V = 12.3) B0.5Ve star located at a distance of ∼ 4.5 kpc.…”

Section: Discussionmentioning

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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Section: Discussionmentioning

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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“…From the occurrence of the two similar single-peaked profile states (in May 2016 and July 2017), we can infer a tentative period of the rotation of the density wave around the star of P dens-wave ∼ 420 d. This period is rather short when compared with periods observed in isolated Be stars, which typically range between five to ten years (Okazaki 1997). However, it has been shown that the V/R quasi periods of Be star discs in Be/XB systems are significantly shorter (Clark et al 1998;Reig et al 2010) owing to the smaller size of the discs in these systems (Reig et al 2016).…”

Section: V/r Variability and Discovery Of A Retrograde One-armed Densmentioning

confidence: 99%

Long-term optical and X-ray variability of the Be/X-ray binary H 1145-619: Discovery of an ongoing retrograde density wave

Alfonso-Garzón

Fabregat

Reig

et al. 2017

A&A

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Context. Multiwavelength monitoring of Be/X-ray binaries is crucial to understand the mechanisms producing their outbursts. H 1145-619 is one of these systems, which has recently displayed X-ray activity. Aims. We investigate the correlation between the optical emission and X-ray activity to predict the occurrence of new X-ray outbursts from the inferred state of the circumstellar disc. Methods. We have performed a multiwavelength study of H 1145-619 from 1973 to 2017 and present here a global analysis of its variability over the last 40 yr. We used optical spectra from the SAAO, SMARTS, and SALT telescopes and optical photometry from the Optical Monitoring Camera (OMC) onboard INTEGRAL and from the All Sky Automated Survey (ASAS). We also used X-ray observations from INTEGRAL/JEM-X, and IBIS to generate the light curves and combined them with Swift/XRT to extract the X-ray spectra. In addition, we compiled archival observations and measurements from the literature to complement these data.Results. Comparing the evolution of the optical continuum emission with the Hα line variability, we identified three different patterns of optical variability: first, global increases and decreases of the optical brightness, observed from 1982 to 1994 and from 2009 to 2017, which can be explained by the dissipation and replenishment of the circumstellar disc; second, superorbital variations with a period of P superorb ≈ 590 days, observed in 2002-2009, which seems to be related to the circumstellar disc; and third, optical outbursts, observed in 1998-1999 and 2002-2005, which we interpret as mass ejections from the Be star. We discovered the presence of a retrograde one-armed density wave, which appeared in 2016 and is still present in the circumstellar disc. Conclusions. We carried out the most complete long-term optical study of the Be/X-ray binary H 1145-619 in correlation with its X-ray activity. For the first time, we found the presence of a retrograde density perturbation in the circumstellar disc of a Be/X-ray binary.

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“…In common with other BeXBs (Reig et al 2005(Reig et al , 2010b, asymmetric profiles are not seen until the disc reaches certain size and density. During the initial stages of disc growth, the shape of the Hα line is always symmetric.…”

Section: Referencesmentioning

confidence: 63%

Disc-loss episode in the Be shell optical counterpart to the high-mass X-ray binary IGR J21343+4738

Reig

Zezas

2014

A&A

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Context. Present X-ray missions are regularly discovering new X-ray and γ-ray sources. The identification of their counterparts at other wavelengths allows us to determine their nature. Aims. The main goal of this work is to determine the properties of the optical counterpart to the INTEGRAL source IGR J21343+4738, and to study its long-term optical variability. Although its nature as a Be/X-ray binary has been suggested, little is known about its physical parameters. Methods. We have been monitoring IGR J21343+4738 since 2009 in the optical band. We present BVRI optical photometric and spectroscopic observations covering the wavelength band 4000-7500 Å. The photometric data allowed us to derive the colour excess E(B − V) and estimate the distance. The blue-end spectra were used to determine the spectral type of the optical companion, while the spectra around the Hα line allowed us to study the long-term structural changes in the circumstellar disc. Results. We find that the optical counterpart to IGR J21343+4738 is a V = 14.1 B1IVe shell star located at a distance of ∼8.5 kpc. The Hα line changed from an absorption-dominated profile to an emission-dominated profile, and then back again into absorption. In addition, fast line profile asymmetries were observed once the disc developed. Although the Balmer lines are the most strongly affected by shell absorption, we find that shell characteristics are also observed in He I lines. Conclusions. The optical spectral variability of IGR J21343+4738 is attributed to the formation of an equatorial disc around the Be star and the development of an enhanced density perturbation that revolves inside the disc. We have witnessed the formation and dissipation of the circumstellar disc. The strong shell profile of the Hα and He I lines and the fact that no transition from the shell phase to a pure emission phase is observed imply that we are seeing the system near edge-on.

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The optical counterpart to IGR J06074+2205: a Be/X-ray binary showing disc loss andV/Rvariability

Cited by 28 publications

References 39 publications

High-mass X-ray binaries in the Milky Way

High-mass X-ray binaries in the Milky Way

Long-term optical and X-ray variability of the Be/X-ray binary H 1145-619: Discovery of an ongoing retrograde density wave

Disc-loss episode in the Be shell optical counterpart to the high-mass X-ray binary IGR J21343+4738

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