SW Sextantis in an excited, low state

Groot, P.; Rutten, R. G. M.; Paradijs, J. van

doi:10.1051/0004-6361:20000483

Cited by 37 publications

(55 citation statements)

References 32 publications

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“…This phase interval and its center coincides with the visibility of a radiating hot-spot on the rim of a geometrically thick accretion disk (e.g. as in IP Peg, Marsh 1988;Groot 1999). Marsh (1988) and Groot et al (2001) have shown the hot-spot to be typically around 10 000 K, corresponding to a late B, early A-type spectrum.…”

Section: Line Light Curvessupporting

confidence: 72%

A spectrophotometric study of RW Trianguli

Groot

Rutten

Paradijs

2004

A&A

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Abstract. On the basis of spectrophotometric observations we reconstruct the accretion disk of the eclipsing novalike cataclysmic variable RW Tri in the wavelength region 3600-7000 Å. We find a radial temperature profile that is, on average, consistent with that expected on the basis of the theory of optically thick, steady state accretion disks and infer a mass-accretion rate in RW Tri of ∼10 −8 M yr −1 . The line emission is dominated by two areas: one around the hot-spot region and one near the white dwarf. Both emission regions have appreciable vertical extension, and seem to be decoupled from the velocity field in the disk. In our observations RW Tri shows a number of features that are characteristic of the SW Sex sub-class of novalike stars. The appearance of a novalike system as a UX UMa/RW Tri or SW Sex star seems to be mainly governed by the mass-transfer rate from the secondary at the time of observation.

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Section: Line Light Curvessupporting

confidence: 72%

A spectrophotometric study of RW Trianguli

Groot

Rutten

Paradijs

2004

A&A

Self Cite

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“…Simulations of stream-disk interaction with inefficient cooling (Armitage & Livio 1998) produce a '' halo '' of material above the disk and a bulge along the disk rim, which can obscure the bright inner disk. This behavior is mainly observed in SW Sex stars (see, e.g., Groot, Rutten, & van Paradijs 2001;Martínez-Pais, Rodríguez-Gil, & Casares 1999), where (possible) magnetic white dwarfs are fed by disk-overflowing material. SW Sex behavior has also been recognized in the neutron star transient XTE J2123À058 during outburst (Hynes et al 2001).…”

Section: Discussionmentioning

confidence: 97%

Bowen Fluorescence from the Companion Star in X1822−371

Casares

Steeghs

Hynes

et al. 2003

ApJ

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We present clear evidence for the motion of the companion star in the low-mass X-ray binary (LMXB) X1822À371. We detect N iii 4640 emission moving in antiphase with the radial velocity curve of the neutron star and produced on the X-ray-heated hemisphere of the donor star. From the motion of this feature we derive a lower limit to the radial velocity semiamplitude of the companion star, K 2 ! 300 AE 8 km s À1 , which, combined with a previous determination of the inclination angle and the pulsar's radial velocity curve, yields M 2 ! 0:36 2 ð Þ M and M 1 ! 1:14 6 ð Þ M . The He i 4471 absorption line moves at lower velocities ('225 km s À1 ) and with a À0.05 phase shift, suggesting a likely origin on the gas stream near the L1 point. In addition, we detect an S-wave emission of O vi 3811 produced by illumination of the hot spot bulge by the central source. The Balmer lines are dominated by broad absorptions probably due to obscuration of the accretion disk by vertically extended cool material from the splash region and overflowing stream. We also derive a more accurate, and significantly different (compared to earlier work), systemic velocity of ¼ À44 AE 5 km s À1 , based on the motion of the He ii 4686 wings and Doppler tomography. This work confirms the power of imaging the companion stars in LMXBs and outbursting transients using the Bowen fluorescence transitions.

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“…Not surprisingly, I Ratio is strongly correlated with the optical flux. Studies performed on accreting white dwarfs have shown some distinctive optical properties when I Ratio is larger than unity as a result of a high ionization 32 . In our analysis we find that strong P-Cyg profiles (blue absorption deeper than 5% of the continuum) are always associated with I Ratio < 1.…”

Section: Ionization Statementioning

confidence: 99%

Regulation of black-hole accretion by a disk wind during a violent outburst of V404 Cygni

Muñoz-Darias

Casares

Sánchez

et al. 2016

Nature

125

164

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Accretion of matter onto black holes is universally associated with strong radiative feedback 1 and powerful outflows 2 . In particular, black hole transients 3 show outflows whose properties 4 are strongly coupled to those of the accretion flow. This includes X-ray winds of ionized material, expelled from the accretion disc encircling the black hole, and collimated radio jets 5,6 . Very recently, a distinct optical variability pattern has been reported in the transient black hole transient V404 Cyg, and interpreted as disrupted mass flow into the inner regions of its large accretion disc 7 . Here, we report on the discovery of a sustained outer accretion disc wind in V404 Cyg, which is unlike any seen previously. We find that the outflowing wind is neutral, has a large covering factor, expands at 1% of the speed of light and triggers a nebular phase once accretion sharply drops and the ejecta become optically thin. The large expelled mass (> l0 -8 M ¤ ) indicates that the outburst was prematurely ended when a sizeable fraction of the outer disc was depleted by the wind, detaching the inner regions from the rest of the disc. The luminous, but brief, accretion phases shown by transients with large accretion discs 2 imply that this outflow is most likely a new fundamental ingredient regulating mass accretion onto black holes.The X-ray binary V404 Cyg (GS 2023+338) is a confirmed stellar-mass BH 8 with a precisely determined distance of 2.4 kpc 9 . Following 25 years of quiescence, the Swift mission detected renewed activity on Jun 15, 2015 10 , initiating a 2-week period of intensely violently variable emission across all wavelengths 11,12 . Our high signal-to-noise GTC optical spectra covering the entire X-ray/radio active phase (~15 days) show that, contemporaneously with radio jet emission, continuous ejections of neutral material at ~0.01c are present from low-level accretion phases (<1% of the Eddington luminosity; L EDD ) to the Xray peak (Methods; Fig. 1, ED Fig. 1). These are observed in hydrogen (Balmer) and helium (He I) emission lines as deep P-Cyg profiles throughout the outburst 13 , and extremely broad wings once the Xray and radio fluxes decay. P-Cyg profiles result from resonant scattering in an expanding outflow with a spherical geometry or at least sustaining a large solid angle 14, 15 (Methods). Among a dozen transitions showing this feature, the deepest are seen in the He I-5876 emission line, which is used as a reference for this study (see ED Fig. 2.).The strongest P-Cyg profiles are witnessed during days 1 to 6 (Fig. 1 and Fig. 2 for the evolution of the profiles during day 2; Methods), when the X-ray luminosity is typically 10 3 times fainter than the ~L EDD flares displayed later in the outburst 7,11 (ED Fig.1). Blue-shifted absorptions are as deep as 30% below the continuum level and we measure terminal velocities in the range V T =1,500 -3,000 km s -1 (Fig. 1, Fig 2, ED Fig 2; ED Fig. 3). Symmetric red-shifted (i.e. positive velocity) outflow emission, completely detached from the accre...

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SW Sextantis in an excited, low state

Cited by 37 publications

References 32 publications

A spectrophotometric study of RW Trianguli

A spectrophotometric study of RW Trianguli

Bowen Fluorescence from the Companion Star in X1822−371

Regulation of black-hole accretion by a disk wind during a violent outburst of V404 Cygni

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