Bowen Fluorescence from the Companion Star in X1822−371

Casares, J.; Steeghs, D.; Hynes, R. I.; Charles, P. A.; O’Brien, Kieran

doi:10.1086/375055

Cited by 50 publications

(106 citation statements)

References 23 publications

(34 reference statements)

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“…The UV/optical spectrum of 4U 1822-371 is rich with emission and absorption lines (Charles et al 1980;Mason & Cordova 1982a;Mason et al 1982;Harlaftis et al 1997;Cowley et al 1982Cowley et al , 2003Jonker et al 2003;Hutchings et al 2005). Doppler tomography of the He II λ4686 and O VI λ3811 emission lines confirms expectations that there is an accretion disk around the neutron star fed by a stream of gas from the secondary star (Casares et al 2003). …”

Section: Introductionsupporting

confidence: 55%

“…There have been several attempts to determine the mass ratio from the radial velocity curve of the secondary star. The spec-trum of the heated face of the secondary star has He I absorption lines and a narrow emission line from N III λ4640, which is excited by the Bowen fluorescence mechanism (Harlaftis et al 1997;Casares et al 2003). The radial velocity curve of the He I absorption has been measured and its amplitude is K HeI ≈ 230 km s −1 (Harlaftis et al 1997;Cowley et al 2003;Casares et al 2003).…”

Section: The Masses and Dimensions Of 4u1822-371mentioning

confidence: 99%

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The Structure of the Accretion Disk in the Accretion Disk Corona X-Ray Binary 4u 1822–371 at Optical and Ultraviolet Wavelengths

Bayless¹,

Robinson²,

Hynes³

et al. 2009

ApJ

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The eclipsing low-mass X-ray binary 4U 1822-371 is the prototypical accretion disk corona (ADC) system. We have obtained new time-resolved UV spectroscopy of 4U 1822-371 with the Advanced Camera for Surveys/Solar Blind Channel on the Hubble Space Telescope and new V -and J-band photometry with the 1.3-m SMARTS telescope at Cerro Tololo Inter-American Observatory. We use the new data to construct its UV/optical spectral energy distribution and its orbital light curve in the UV, V , and J bands. We derive an improved ephemeris for the optical eclipses and confirm that the orbital period is changing rapidly, indicating extremely high rates of mass flow in the system; and we show that the accretion disk in the system has a strong wind with projected velocities -2 -up to 4000 km s −1 . We show that the disk has a vertically-extended, opticallythick component at optical wavelengths. This component extends almost to the edge of the disk and has a height equal to ∼0.5 of the disk radius. As it has a low brightness temperature, we identify it as the optically-thick base of a disk wind, not as the optical counterpart of the ADC. Like previous models of 4U 1822-371, ours needs a tall obscuring wall near the edge of the accretion disk, but we interpret the wall as a layer of cooler material at the base of the disk wind, not as a tall, luminous disk rim.

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Section: Introductionsupporting

confidence: 55%

Section: The Masses and Dimensions Of 4u1822-371mentioning

confidence: 99%

The Structure of the Accretion Disk in the Accretion Disk Corona X-Ray Binary 4u 1822–371 at Optical and Ultraviolet Wavelengths

Bayless¹,

Robinson²,

Hynes³

et al. 2009

ApJ

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“…For example, Steeghs & Casares (2002) detected a large number of very narrow emission line features from the irradiated secondary star in the persistent X-ray binary Sco X-1. Furthermore, the discovery of sharp emission components of the Bowen blend in Sco X-1 and the X-ray transient GX 339-4 caught in an outburst state allowed the determination of the primary masses (Steeghs & Casares 2002;Casares et al 2003;Hynes et al 2003;Muñoz-Darias et al 2008).…”

Section: Introductionmentioning

confidence: 99%

Spectroscopic evidence for a low-mass black hole in SWIFT J1753.5−0127

Neustroev

Veledina

Poutanen

et al. 2014

Monthly Notices of the Royal Astronomical Society

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The black hole (BH) candidate SWIFT J1753.5-0127 has remained active since the onset of its 2005 outburst. Emission lines in the optical spectrum were observed at the very beginning of the outburst, but since then the spectrum has been featureless making a precise BH mass estimation impossible. Here we present results from our optical and ultraviolet (UV) observations of SWIFT J1753.5-0127 taken in 2012-2013. Our new observations show extremely broad, double-peaked emission lines in the optical and UV spectra. The optical data also show narrow absorption and emission features with nearly synchronous and significant Doppler motions. A radial velocity study of these lines which we associate with the secondary star, yields a semi-amplitude of K 2 =382 km s −1 . A time-series analysis of the spectral and photometric data revealed a possible orbital periodicity of 2.85 h, significantly shorter than the reported 3.2 h periodic signal by Zurita et al. The observed variability properties argue against a low orbital inclination angle and we present several observational arguments in favour of the BH interpretation. However, the measured radial velocity semi-amplitude of the donor star and the short orbital period imply that SWIFT J1753.5-0127 has one of the lowest measured mass function for a BH in a low-mass X-ray binary. We show that the compact object mass in excess of 5 M ⊙ is highly improbable. Thus, SWIFT J1753.5-0127 is a BH binary that has one of the shortest orbital period and hosts probably one of the smallest stellar mass BH found to date.

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“…From the X-ray pulse arrival times Jonker & van der Klis (2001) were able to determine that the orbit of the system is almost circular and that the mass function of the neutron star is (2.03±0.03)×10 −2 M . Casares et al (2003) detected Bowen fluorescence from the secondary star and constrained the lower limit of the radial velocity semiamplitude of the secondary to be 300 ± 8 km s −1 . This combined with the radial Article published by EDP Sciences A111, page 1 of 10 velocity semiamplitude of the neutron star (calculated from the projected semi-major axis of the NS by Jonker & van der Klis 2001) constrains the lower limits for the component masses M 2 > 0.36 M and M 1 > 1.14 M (Casares et al 2003).…”

Section: Introductionmentioning

confidence: 99%

Phase-resolved optical and X-ray spectroscopy of low-mass X-ray binary X1822–371

Somero

Hakala

Muhli

et al. 2012

A&A

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Context. X1822-371 is the prototypical accretion disc corona X-ray source, a low-mass X-ray binary viewed at very high inclination, thereby allowing the disc structure and extended disc coronal regions to be visible. As the brightest (closest) such source, X1822-371 is ideal for studying the shape and edge structure of an accretion disc, and comparing with detailed models. Aims. We study the structure of the accretion disc in X1822-371 by modelling the phase-resolved spectra both in optical and X-ray regime. Methods. We analyse high time resolution optical ESO/VLT spectra of X1822-371 to study the variability in the emission line profiles. In addition, we use data from XMM-Newton space observatory to study phase-resolved as well as high resolution X-ray spectra. We apply the Doppler tomography technique to reconstruct a map of the optical emission distribution in the system. We fit multi-component models to the X-ray spectra. Results. We find that our results from both the optical and X-ray analysis can be explained with a model where the accretion disc has a thick rim in the region where the accretion stream impacts the disc. The behaviour of the Hβ line complex implies that some of the accreting matter creates an outburst around the accretion stream impact location and that the resulting outflow of matter moves both away from the accretion disc and towards the centre of the disc. Such behaviour can be explained by an almost isotropic outflow of matter from the accretion stream impact region. The optical emission lines of He ii λ4686 and 5411 show double peaked profiles, typical for an accretion disc at high inclination. However, their velocities are slower than expected for an accretion disc in a system like X1822-371. This, combined with the fact that the He ii emission lines do not get eclipsed during the partial eclipse in the continuum, suggests that the line emission does not originate in the orbital plane and is more likely to come from above the accretion disc, for example the accretion disc wind.

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Bowen Fluorescence from the Companion Star in X1822−371

Cited by 50 publications

References 23 publications

The Structure of the Accretion Disk in the Accretion Disk Corona X-Ray Binary 4u 1822–371 at Optical and Ultraviolet Wavelengths

The Structure of the Accretion Disk in the Accretion Disk Corona X-Ray Binary 4u 1822–371 at Optical and Ultraviolet Wavelengths

Spectroscopic evidence for a low-mass black hole in SWIFT J1753.5−0127

Phase-resolved optical and X-ray spectroscopy of low-mass X-ray binary X1822–371

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