Orbital periods of cataclysmic variables identified by the SDSS

Southworth, J.; Hickman, Richard; Marsh, T. R.; Rebassa‐Mansergas, A.; Gänsicke, B. T.; Copperwheat, C. M.; Rodríguez‐Gil, P.

doi:10.1051/0004-6361/200912885

Cited by 26 publications

(17 citation statements)

References 61 publications

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“…D'Avanzo et al () observed Hα emission from the leading side of the inner face of the companion star in Cen X‐4 and attributed it to irradiation from the hotspot and shielding from the gas stream. Southworth et al () observed Hα emission from the secondary of J100658.40+233724.4. González Hernández & Casares () detected Hα emission from the secondary of the black hole system A0620−00 which they attributed to chromospheric activity induced by rapid rotation.…”

Section: Discussionmentioning

confidence: 99%

A tomographic study of V691 CrA (X1822−371)

Peris

Vrtilek

2012

Monthly Notices of the Royal Astronomical Society

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We present Doppler and modulation tomography of the low‐mass X‐ray binary V691 CrA with data obtained using the 6.5‐m Magellan Baade telescope at the Las Campanas Observatory in 2010 and 2011. The disc and hotspot are observed in Hα and He ii (λ4686) in both years. A clear image of the disc is seen in He ii (λ5411) using the 2010 data. We present the first tomography of the absorption line He i (λ5876) and detect absorption near the L1 point of the donor star. We also present the first modulation tomography of the emission line Hα and detect emission from the secondary. The Hα double peaks are imbedded in a deep absorption trough confirming the presence of Balmer line absorbing material in the system. Our observations of Hα show absorption in a larger phase range than in Hβ which could be due to heating up of sprayed matter from the hotspot as it travels downstream. We also suggest possible occultation of the Hα absorbing spray by the disc bulge at certain phases.

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Section: Discussionmentioning

confidence: 99%

A tomographic study of V691 CrA (X1822−371)

Peris

Vrtilek

2012

Monthly Notices of the Royal Astronomical Society

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“…Notably, Mukadam et al (2011) used this information to discovered the only known outburst of CV SDSS J074531.92+453829.6. Similarly, Southworth et al (2009) used the data to find and constrain the rate of outbursts for eclipsing CV SDSSJ100658.40+233724.4.…”

Section: Photometric Follow-upmentioning

confidence: 99%

Cataclysmic variables from the Catalina Real-time Transient Survey

Drake

Gänsicke

Djorgovski

et al. 2014

Monthly Notices of the Royal Astronomical Society

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102

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We present 855 cataclysmic variable candidates detected by the Catalina Real-time Transient Survey (CRTS) of which at least 137 have been spectroscopically confirmed and 705 are new discoveries. The sources were identified from the analysis of five years of data, and come from an area covering three quarters of the sky. We study the amplitude distribution of the dwarf novae CVs discovered by CRTS during outburst, and find that in quiescence they are typically two magnitudes fainter compared to the spectroscopic CV sample identified by SDSS. However, almost all CRTS CVs in the SDSS footprint have ugriz photometry. We analyse the spatial distribution of the CVs and find evidence that many of the systems lie at scale heights beyond those expected for a Galactic thin disc population. We compare the outburst rates of newly discovered CRTS CVs with the previously known CV population, and find no evidence for a difference between them. However, we find that significant evidence for a systematic difference in orbital period distribution. We discuss the CVs found below the orbital period minimum and argue that many more are yet to be identified among the full CRTS CV sample. We cross-match the CVs with archival X-ray catalogs and find that most of the systems are dwarf novae rather than magnetic CVs.

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“…In this section we provide a concise description of the code, LCURVE, that we wrote in order to model the light-curves of this paper; the same code has been used in Pyrzas et al (2009) and Southworth et al (2009). The aim of the code was to provide a flexible framework for fitting light-curves characteristic of eclipsing dwarf novae and detached white dwarf / M dwarf binary stars.…”

Section: Discussionmentioning

confidence: 99%

Physical properties of IP Pegasi: an eclipsing dwarf nova with an unusually cool white dwarf

Copperwheat¹,

Marsh²,

Dhillon³

et al. 2011

Proceedings of High Time Resolution Astrophysics (HTRA) IV - The Era of Extremely Large Telescopes — PoS(HTRA-IV)

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We present high speed photometric observations of the eclipsing dwarf nova IP Peg taken with the triple-beam camera ULTRACAM mounted on the William Herschel Telescope. The primary eclipse in this system was observed twice in 2004, and then a further sixteen times over a three week period in 2005. Our observations were simultaneous in the Sloan u ′ , g ′ and r ′ bands. By phase-folding and averaging our data we make the first significant detection of the white dwarf ingress in this system and find the phase width φ of the white dwarf eclipse to be 0.0935 ± 0.0003, significantly higher than the previous best value of 0.0863 < φ < 0.0918. The mass ratio is found to be q = M 2 /M 1 = 0.48 ± 0.01, consistent with previous measurements, but we find the inclination to be 83.8 ± 0.5 deg, significantly higher than previously reported. We find the radius of the white dwarf to be 0.0063 ± 0.0003R ⊙ , implying a white dwarf mass of 1.16 ± 0.02M ⊙ . The donor mass is 0.55 ± 0.02M ⊙ . The white dwarf temperature is more difficult to determine, since the white dwarf is seen to vary significantly in flux, even between consecutive eclipses. This is seen particularly in the u ′ -band, and is probably the result of absorption by disc material. Our best estimate of the temperature is 10, 000 -15, 000K, which is much lower than would be expected for a CV with this period, and implies a mean accretion rate of < 5 × 10 −11 M ⊙ yr −1 , more than 40 times lower than the expected rate.

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Orbital periods of cataclysmic variables identified by the SDSS

Cited by 26 publications

References 61 publications

A tomographic study of V691 CrA (X1822−371)

A tomographic study of V691 CrA (X1822−371)

Cataclysmic variables from the Catalina Real-time Transient Survey

Physical properties of IP Pegasi: an eclipsing dwarf nova with an unusually cool white dwarf

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