Time-resolved, multi-color photometry and spectroscopy   of Virgo 4 (OU Vir): A high orbital inclination, short orbital period dwarf nova

Mason, E.; Howell, Steve B.; Szkody, Paula; Harrison, T. E.; Holtzman, Jon A.; Hoard, D. W.

doi:10.1051/0004-6361:20021446

Cited by 7 publications

(5 citation statements)

References 23 publications

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“…OU Vir was observed during descent from superoutburst in both 2002 and 2003. Mason et al (2002) found that for OU Vir out of eclipse and during quiescence, V = 18.08 and B − V = 0.14, which corresponds to g ′∼ 0.2 mJy (Smith et al 2002). Vanmunster et al (2000) quote an outburst amplitude of approximately 4 mag (corresponding to a peak g ′ flux of ∼8.4 mJy).…”

Section: Light‐curve Morphologymentioning

confidence: 99%

“…OU Vir is a faint ( V ∼ 18; Mason et al 2002) eclipsing CV with a period of 1.75 hr which has been seen in outburst and probably superoutburst (Vanmunster, Velthuis & McCormick 2000), marking it as an SU UMa dwarf nova. Mason et al (2002) presented time‐resolved, multicolour photometry and spectroscopy of OU Vir, concluding that the eclipse is of the bright spot and the disc, but not of the white dwarf. In this paper, we present light curves of OU Vir, obtained with ULTRACAM, an ultra‐fast, triple‐beam CCD camera; for more details, see Dhillon & Marsh (2001); Dhillon et al (in preparation).…”

Section: Introductionmentioning

confidence: 99%

“…OU Vir is a faint (V ∼ 18; Mason et al 2002) eclipsing CV with a period of 1.75 hr which has been seen in outburst and probably superoutburst (Vanmunster et al 2000), marking it as a SU UMa dwarf nova. Mason et al (2002) presented time-resolved, multi-colour photometry and spectroscopy of OU Vir, concluding that the eclipse is of the bright spot and disc, but not the white dwarf.…”

Section: Introductionmentioning

confidence: 99%

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ULTRACAM photometry of the eclipsing cataclysmic variable OU Vir

Feline

Dhillon

Marsh

et al. 2004

Monthly Notices of the Royal Astronomical Society

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We present high-speed, three-colour photometry of the faint eclipsing cataclysmic variable OU Vir. For the first time in OU Vir, separate eclipses of the white dwarf and bright spot have been observed. We use timings of these eclipses to derive a purely photometric model of the system, obtaining a mass ratio of q = 0.175 +/- 0.025, an inclination of i = 79.2 +/- 0.7 degrees and a disc radius of Rd/a = 0.2315 +/- 0.0150. We separate the white dwarf eclipse from the lightcurve and, by fitting a blackbody spectrum to its flux in each passband, obtain a white dwarf temperature of T = 21700 +/- 1200 K and a distance of D = 650 +/- 210 pc. Assuming that the primary obeys the Nauenberg (1972) mass-radius relation for white dwarfs and allowing for temperature effects, we also find a primary mass Mw/Msun = 0.90 +/- 0.19, primary radius Rw/Rsun = 0.0097 +/- 0.0031 and orbital separation a/Rsun = 0.75 +/- 0.05.Comment: 8 pages LaTeX, 6 figures. Accepted by MNRAS; erratum added at end. Mon.Not.Roy.Astron.Soc. 347 (2004) 1173, erratum in pres

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Section: Light‐curve Morphologymentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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ULTRACAM photometry of the eclipsing cataclysmic variable OU Vir

Feline

Dhillon

Marsh

et al. 2004

Monthly Notices of the Royal Astronomical Society

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“…The light curve for V446 Her shows a brightening in all three bands, followed by a sudden drop. The morphology and amplitude of these variations are very similar to those seen in the optical light curves of OU Vir (Mason et al 2002). Mason et al explain those light curves by invoking a high inclination system (60 • ≤ i ≤ < 70 • ) with a large, optically thick accretion disk hot spot.…”

Section: The Light Curves Of V1974 Cygni V446 Herculis Qv Vulpeculae ...mentioning

confidence: 54%

Phase-Resolved Infrared Spectroscopy and Photometry of V1500 Cygni, and a Search for Similar Old Classical Novae

Harrison

Campbell

Lyke

2013

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We present phase-resolved near-infrared photometry and spectroscopy of the classical nova V1500 Cyg to explore whether cyclotron emission is present in this system. While the spectroscopy do not indicate the presence of discrete cyclotron harmonic emission, the light curves suggest that a sizable fraction of its near-infrared fluxes are due to this component. The light curves of V1500 Cyg appear to remain dominated by emission from the heated face of the secondary star in this system. We have used infrared spectroscopy and photometry to search for other potential magnetic systems amongst old classical novae. We have found that the infrared light curves of V1974 Cyg superficially resemble those of V1500 Cyg, suggesting a highly irradiated companion. The old novae V446 Her and QV Vul have light curves with large amplitude variations like those seen in polars, suggesting they might have magnetic primaries. We extract photometry for seventy nine old novae from the 2MASS Point Source Catalog and use those data to derive the mean, un-reddened infrared colors of quiescent novae. We also extract W ISE data for these objects and find that forty five of them were detected. Surprisingly, a number of these systems were detected in the W ISE 22 µm band. While two of those objects produced significant dust shells (V705 Cas and V445 Pup), the others did not. It appears that line emission from their ionized ejected shells is the most likely explanation for those detections.

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“…This hotspot is where the accretion stream from the secondary impacts the disk. These spots typically have temperatures of 20,000 K, and can produce modulations on order of ±50% in visible bandpasses (Mason et al 2002). Because this feature is on the outer edge of the disk, it has the potential to distort the reflex motions in systems where it is prominent.…”

Section: Sco X-1mentioning

confidence: 99%

Modeling Multi-Wavelength Stellar Astrometry. I. Sim Lite Observations of Interacting Binaries

Coughlin

Gelino

Harrison

et al. 2010

ApJ

Self Cite

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Interacting binaries consist of a secondary star which fills or is very close to filling its Roche lobe, resulting in accretion onto the primary star, which is often, but not always, a compact object. In many cases, the primary star, secondary star, and the accretion disk can all be significant sources of luminosity. SIM Lite will only measure the photocenter of an astrometric target, and thus determining the true astrometric orbits of such systems will be difficult. We have modified the Eclipsing Light Curve code (Orosz & Hauschildt 2000) to allow us to model the flux-weighted reflex motions of interacting binaries, in a code we call reflux. This code gives us sufficient flexibility to investigate nearly every configuration of interacting binary. We find that SIM Lite will be able to determine astrometric orbits for all sufficiently bright interacting binaries where the primary or secondary star dominates the luminosity. For systems where there are multiple components that comprise the spectrum in the optical bandpass accessible to SIM Lite, we find it is possible to obtain absolute masses for both components, although multi-wavelength photometry will be required to disentangle the multiple components. In all cases, SIM Lite will at least yield accurate inclinations, and provide valuable information that will allow us to begin to understand the complex evolution of mass-transferring binaries. It is critical that SIM Lite maintains a multi-wavelength capability to allow for the proper deconvolution of the astrometric orbits in multi-component systems.

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Time-resolved, multi-color photometry and spectroscopy of Virgo 4 (OU Vir): A high orbital inclination, short orbital period dwarf nova

Cited by 7 publications

References 23 publications

ULTRACAM photometry of the eclipsing cataclysmic variable OU Vir

ULTRACAM photometry of the eclipsing cataclysmic variable OU Vir

Phase-Resolved Infrared Spectroscopy and Photometry of V1500 Cygni, and a Search for Similar Old Classical Novae

Modeling Multi-Wavelength Stellar Astrometry. I. Sim Lite Observations of Interacting Binaries

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