Optical and infrared light curves of the eclipsing X-ray binary V395 Car = 2S 0921−630

Ashcraft, Teresa; Hynes, R. I.; Robinson, E. L.

doi:10.1111/j.1365-2966.2012.21241.x

Cited by 7 publications

(3 citation statements)

References 16 publications

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“…The Hard X-ray Detector (HXD-PIN; Takahashi et al 2007) 𝑏 Average count rate for XIS0, XIS1, and XIS3 for 0.5-10 keV energy range. 𝑐 Orbital phase based on the ephemeris of Ashcraft et al (2012).…”

Section: Observationsmentioning

confidence: 99%

“…The top and middle panels show the XIS and HXD-PIN light curves with corresponding hardness ratio in the bottom panel. The observations cover the orbital phases of 0.31-0.44, 0.56-0.68, 0.86-0.98, and 1.04-1.16, respectively, based on the ephemeris of Ashcraft et al (2012) with phase zero at the centre of the eclipse. X-ray flux is variable across the four epochs.…”

Section: Light Curvementioning

confidence: 99%

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Broad-band spectral analysis of LMXB 2S 0921-63 with Suzaku

Sharma

Jain

Dutta

2022

Monthly Notices of the Royal Astronomical Society

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We present the broad-band spectral analysis of the low-mass X-ray binary 2S 0921-63 by using the Suzaku archival data covering the orbital phase between 0.31 and 1.16 during four close observations. It is the first time that a broad-band spectral analysis of 2S 0921-63 has been done up to 25 keV. The 0.5–10 keV XIS count rate varied between ∼ 1 and ∼ 5 counts s−1 during the observations. A partial X-ray eclipse and broad post-eclipse intensity dip were observed during the observations. The X-ray emission hardened marginally during the intensity dip. We have modelled the source spectra by simultaneously fitting the XIS and HXD-PIN spectra for each of the four observations. The broad-band spectra of the source can be described by a model comprising a very hot blackbody having temperature, kTBB ≈ 1.66 − 2.13 keV, a high-energy cutoff power law, and an Fe emission line at Eline ∼ 6.7 keV. A second model, accounting for the Comptonization of the thermal emission from accretion disc along with an Fe emission line, describes the broad-band spectra of 2S 0921-63 equally well.

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Section: Observationsmentioning

confidence: 99%

Section: Light Curvementioning

confidence: 99%

Broad-band spectral analysis of LMXB 2S 0921-63 with Suzaku

Sharma

Jain

Dutta

2022

Monthly Notices of the Royal Astronomical Society

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“…Less well-known giant LMXB systems include V395 Car = 2S 0921−630 with an orbital period of 9.0 days and accretion disk eclipses. The NS mass is 1.44 ± 0.10 M e with a companion mass of 0.35 ± 0.03 M e (Ashcraft et al 2012). The secondary has been identified as a ~50 L e lowluminosity K0 III (Shahbaz et al 1999).…”

Section: Low-mass X-ray Binariesmentioning

confidence: 99%

On Its Way to the Neutron Star–White Dwarf Binary Graveyard, IGR J16194−2810, A First Ascent M Giant X-Ray Binary

Hinkle,

Fekel,

Straniero

et al. 2024

ApJ

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A single-lined spectroscopic orbit for the M giant in the X-ray binary IGR J16194−2810 is determined from a time series of optical spectra. The spectroscopic orbital period of 192.5 days is twice that of the photometric period, confirming that the M giant in the system is an ellipsoidal variable. The giant is identified as a first ascent giant approaching the red giant tip. The primary is a neutron star (NS) with its M giant companion filling its Roche lobe, verifying the system classification as a low-mass X-ray binary (LMXB). Stellar C, N, O, and Fe abundances are derived for the M giant with the C, N, and O values typical for a field giant with [Fe/H] = −0.14. The system does not have a large kick velocity. Models for the evolution of the system into a binary NS–white dwarf are presented. The X-ray properties are discussed in the context of this model. This binary is a rare example of a luminous, long orbital period LMXB early in the transient ellipsoidal phase.

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A different view of wind in X-ray binaries: the accretion disc corona source 2S 0921-630

Tomaru

Done

Odaka

et al. 2023

Monthly Notices of the Royal Astronomical Society

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Accretion disc coronae (ADC) sources are very high inclination neutron star or black hole binaries, where the outer accretion flow blocks a direct view of the central source. The weak observed X-ray emission is instead produced mainly by scattering of the intrinsic radiation from highly ionised gas surrounding the source, the ADC. However, the origin of this scattering material is still under debate. We use the ADC source 2S 0921-630 (V395 Car) to test whether it is consistent with a thermal-radiative wind produced by the central X-ray source illuminating and puffing up the outer disc. This wind is clearly visible in blueshifted absorption lines in less highly inclined systems, where the source is seen directly through this material. Using the phenomenological photoionised plasma model, we first characterise the parameter that drives emission lines observed in 2S0921 in XMM-Newton and Chandra data. Following this, we run the Monte Carlo radiation transfer simulation to get scattered/reprocessed emissions in the wind, with the density and velocity structure obtained from the previous work. Our model agrees with all the wind emission lines in the Chandra high and medium energy grating spectra for an intrinsic source luminosity of L > 0.2 LEdd. This result strongly favours thermal-radiative winds as the origin of the ADC. We also show how high-resolution spectra via microcalorimeters can provide a definitive test by detecting blueshifted absorption lines.

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Optical and infrared light curves of the eclipsing X-ray binary V395 Car = 2S 0921−630

Cited by 7 publications

References 16 publications

Broad-band spectral analysis of LMXB 2S 0921-63 with Suzaku

Broad-band spectral analysis of LMXB 2S 0921-63 with Suzaku

On Its Way to the Neutron Star–White Dwarf Binary Graveyard, IGR J16194−2810, A First Ascent M Giant X-Ray Binary

A different view of wind in X-ray binaries: the accretion disc corona source 2S 0921-630

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