The phase 0.5 absorption in V1315 Aquilae, SW Sextantis, and DW Ursae Majoris

Szkody, Paula; Piche, Francois

doi:10.1086/169188

Cited by 35 publications

(34 citation statements)

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“…If the mass-transfer rate from the secondary is larger than observed here for SW Sex it is well possible that a larger amount of the mass is transferred to the inner disk which may cause the veiling. Back-lighting by the hot-spot continuum radiation certainly explains the phase-dependence of the absorption features which have been shown to have maximum depth around ϕ ∼0.45, exactly when we see the hot-spot region from across the disk (Szkody & Piché, 1990). -Shallow eclipses of the emission lines.…”

Section: The Sw Sex Phenomenon Explained (?)supporting

confidence: 60%

SW Sextantis in an excited, low state

Groot

Rutten

Paradijs

2001

A&A

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Abstract. We present low-resolution spectrophotometric optical observations of the eclipsing nova-like cataclysmic variable SW Sex, the prototype of the SW Sex stars. We observed the system when it was in an unusual low state. The spectrum is characterized by the presence of strong Heii and Civ emission lines as well as the normal single peaked Balmer emission lines. The radial temperature profile of the disk follows the expected T∝R −3/4 only in the outer parts and flattens off inside 0.5 times the white dwarf Roche lobe radius. The single peaked emission lines originate in a region above the plane of the disk, at the position of the hot spot.

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Section: The Sw Sex Phenomenon Explained (?)supporting

confidence: 60%

SW Sextantis in an excited, low state

Groot

Rutten

Paradijs

2001

A&A

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“…This absorption is apparent from phases 0.43 to 0.57 and is strongest at phase 0.54. This absorption is an indication of a SW Sex star (Szkody & Piché 1990); however, it is not as deep as in other SW Sex stars such as DW UMa (Szkody & Piché 1990), BH Lyn (Hoard & Szkody 1997), and V1315 Aql (Dhillon, Marsh, & Jones 1991). In these stars, absorption can be below the continuum in the higher order Balmer and He i lines.…”

Section: Spectroscopymentioning

confidence: 89%

Investigating the Sloan Digital Sky Survey Cataclysmic Variable SDSS J132723.39+652854.2

Wolfe¹,

Szkody²,

Fraser³

et al. 2003

PUBL ASTRON SOC PAC

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ABSTRACT. Photometric and spectroscopic observations reveal the Sloan Digital Sky Survey cataclysmic variable SDSS J132723.39ϩ652854.2 to be a likely SW Sex star with an orbital period of hr. The P p 3.28 Sloan Digital Sky Survey spectrum shows strong He i, He ii, and Balmer emission lines. Time-resolved spectra acquired at Apache Point Observatory reveal absorption-line structure within the emission lines near phase 0.5. Photometric data obtained at Manastash Ridge Observatory using Harris V and B filters reveal a high-inclination system ( ) with deep (∼2 mag) eclipses. The orbital period and the spectral variations favor an SW Sex i p 80Њ interpretation.

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“…A quarter century ago, a sub-class of NLs, called "SW Sex stars", was identified (Szkody & Piche 1990;Thorstensen et al 1991a;Dhillon et al 2013) with contradictory properties: deep continuum eclipses (with unusual V-shaped profiles) that imply a high-inclination accretion disc and emission lines with singlepeaked profiles and shallow eclipses, instead of the deeply eclipsing, double-peaked profiles one would expect (Horne & Marsh 1986). Moreover, their emission lines do not reflect the orbital motion of the white dwarf (there is a substantial orbital phase lag of ∼0.2 cycle) and exhibit transient absorption features around phase 0.5, all indicative of a complex, possibly non-disk origin.…”

Section: Introductionmentioning

confidence: 99%

2MASS J22560844+5954299: the newly discovered cataclysmic star with the deepest eclipse

Kjurkchieva

Khruzina

Dimitrov

et al. 2015

A&A

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Context. The SW Sex stars are assumed to represent a distinguished stage in cataclysmic variable (CV) evolution, making it especially important to study them. Aims. We discovered a new cataclysmic star and carried out prolonged and precise photometric observations, as well as mediumresolution spectral observations. Modelling these data allowed us to determine the physical parameters and to establish its peculiarities. Methods. To obtain a light curve solution we used model whose emission sources are a white dwarf surrounded by an accretion disk with a hot spot, a gaseous stream near the disk's lateral side, and a secondary star filling its Roche lobe. The obtained physical parameters are compared with those of other SW Sex-subtype stars. Results. The newly discovered cataclysmic variable 2MASS J22560844+5954299 shows the deepest eclipse amongst the known nova-like stars. It was reproduced by totally covering a very luminous accretion disk by a red secondary component. The temperature distribution of the disk is flatter than that of steady-state disk. The target is unusual with the combination of a low mass ratio q ∼ 1.0 (considerably below the limit q = 1.2 of stable mass transfer of CVs) and an M-star secondary. The intensity of the observed three emission lines, Hα, He 5875, and He 6678, sharply increases around phase 0.0, accompanied by a Doppler jump to the shorter wavelength. The absence of eclipses of the emission lines and their single-peaked profiles means that they originate mainly in a vertically extended hot-spot halo. The emission Hα line reveals S-wave wavelength shifts with semi-amplitude of around 210 km s −1 and phase lag of 0.03. Conclusions. The non-steady-state emission of the luminous accretion disk of 2MASS J22560844+5954299 was attributed to the low viscosity of the disk matter caused by its unusually high temperature. The star shows all spectral properties of an SW Sex variable apart from the 0.5 central absorption.

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The phase 0.5 absorption in V1315 Aquilae, SW Sextantis, and DW Ursae Majoris

Cited by 35 publications

References 0 publications

SW Sextantis in an excited, low state

SW Sextantis in an excited, low state

Investigating the Sloan Digital Sky Survey Cataclysmic Variable SDSS J132723.39+652854.2

2MASS J22560844+5954299: the newly discovered cataclysmic star with the deepest eclipse

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