Optical spectroscopy of the massive X-ray binary QV Nor (4U 1538 - 52)*

Reynolds, A. P.; Bell, S. A.; Hilditch, R. W.

doi:10.1093/mnras/256.4.631

Cited by 49 publications

(56 citation statements)

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“…The companion is a B0I star located at 5.5 kpc (Becker et al, 1977;Reynolds et al, 1992). Variability of the absorption at eclipse egress allows to measure the stellar wind parameters (Clark et al, 1994).…”

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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“…The parameter β = 0.8−1.2 is the velocity gradient for an OB supergiant (Friend & Abbott 1986), and R = 17.2 R (Reynolds et al 1992), the radius of the donor. The resulting N H arises from the integration of n H (r) along the line of sight.…”

Section: The Stellar Wind In 4u 1538−52mentioning

confidence: 99%

“…It also depends on the distance between both components and the stellar wind velocity, for the most part. The estimated X-ray luminosity is ∼(2.6−9.1) × 10 36 erg s −1 in the 3−100 keV range, assuming an isotropic emission and a distance of 6.4 kpc Article published by EDP Sciences A140, page 1 of 5 (Reynolds et al 1992). Thus, the analysis of the X-ray spectrum from the neutron star at different orbital phases provides us the variability of the model parameters we can use to compare with accretion models.…”

Section: Introductionmentioning

confidence: 99%

Orbital phase-resolved spectroscopy of 4U 1538−52 with MAXI

Roca

Mihara

Nakahira

et al. 2015

A&A

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Context. 4U 1538−52, an absorbed high mass X-ray binary with an orbital period of ∼3.73 days, shows moderate orbital intensity modulations with a low level of counts during the eclipse. Several models have been proposed to explain the accretion at different orbital phases by a spherically symmetric stellar wind from the companion. Aims. The aim of this work is to study both the light curve and orbital phase spectroscopy of this source in the long term. In particular, we study the folded light curve and the changes in the spectral parameters with orbital phase to analyse the stellar wind of QV Nor, the mass donor of this binary system. Methods. We used all the observations made from the Gas Slit Camera on board MAXI of 4U 1538−52 covering many orbits continuously. We obtained the good interval times for all orbital phase ranges, which were the input for extracting our data. We estimated the orbital period of the system and then folded the light curves, and we fitted the X-ray spectra with the same model for every orbital phase spectrum. We also extracted the averaged spectrum of all the MAXI data available. Results. The MAXI spectra in the 2-20 keV energy range were fitted with an absorbed Comptonisation of cool photons on hot electrons. We found a strong orbital dependence of the absorption column density but neither the fluorescence iron emission line nor low energy excess were needed to fit the MAXI spectra. The variation in the spectral parameters over the binary orbit were used to examine the mode of accretion onto the neutron star in 4U 1538−52. We deduce a best value ofṀ/v ∞ = 0.65 × 10 −9 M yr −1 /(km s −1 ) for QV Nor.

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“…With M = 1.3 M (Reynolds et al 1992), M 17 = 883 g s −1 (Clark et al 1994;Rodes 2007;Rodes et al 2008), and μ 30 = 1.8 G cm 3 (Rodes 2007), the Eq. (3) yields the value R m ∼ 6.2 × 10 7 cm.…”

Section: X-ray Continuummentioning

confidence: 99%

Detecting emission lines withXMM-Newtonin 4U 1538–52

Roca

Page

Torrejón

et al. 2010

A&A

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Context. The properties of the X-ray emission lines are a fundamental tool for studying the nature of the matter surrounding the neutron star and the phenomena that produce these lines. Aims. The aim of this work is to analyse the X-ray spectrum of 4U 1538−52 obtained by the XMM-Newton observatory and to look for the presence of diagnostic lines in the energy range 0.3−11.5 keV. Methods. We used a 54 ks PN & MOS/XMM-Newton observation of the high-mass X-ray binary 4U 1538−52 covering the orbital phase between 0.75 to 1.00 (the eclipse ingress). We modelled the 0.3−11.5 keV continuum emission with three absorbed power laws and looked for the emission lines. Results. We found previously unreported recombination lines in this system at ∼2.4 keV, ∼1.9 keV, and ∼1.3 keV, which is consistent with the presence of highly ionized states of S XV Heα, Si XIII Heα, and either Mg Kα or Mg XI Heα. On the other hand, in spectra that are both out of eclipse and in eclipse, we detect a fluorescence iron emission line at 6.4 keV, which is resolved into two components: a narrow (σ ≤ 10 eV) fluorescence Fe Kα line plus one hot line from highly photoionized Fe XXV. Conclusions. The detection of new recombination lines during eclipse ingress in 4U 1538−52 indicates that there is an extended ionized region surrounding the neutron star.

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Optical spectroscopy of the massive X-ray binary QV Nor (4U 1538 - 52)*

Cited by 49 publications

References 0 publications

High-mass X-ray binaries in the Milky Way

High-mass X-ray binaries in the Milky Way

Orbital phase-resolved spectroscopy of 4U 1538−52 with MAXI

Detecting emission lines withXMM-Newtonin 4U 1538–52

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