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Title:
Observations of V592 Cassiopeiae with the Spitzer Space Telescope—Dust in the Mid-Infrared
Authors:
Hoard, D. W.; Kafka, Stella; Wachter, Stefanie; Howell, Steve B.; Brinkworth, Carolyn S.; Ciardi, David R.; Szkody, Paula; Belle, Kunegunda; Froning, Cynthia; van Belle, Gerard
Affiliation:
AA( Spitzer Science Center, California Institute of Technology, Pasadena, CA 91125, USA ), AB( Spitzer Science Center, California Institute of Technology, Pasadena, CA 91125, USA ), AC( Spitzer Science Center, California Institute of Technology, Pasadena, CA 91125, USA ), AD(National Optical Astronomy Observatory, Tucson, AZ 85719, USA ), AE( Spitzer Science Center, California Institute of Technology, Pasadena, CA 91125, USA ), AF(Michelson Science Center, California Institute of Technology, Pasadena, CA 91125, USA ), AG(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195-1580, USA ), AH(X-4 MS T085, Los Alamos National Laboratory, Los Alamos, NM 87545, USA ), AI(Center for Astrophysics and Space Astronomy, University of Colorado, 593 UCB, Boulder, CO 80309, USA ), AJ(European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany)
Publication:
The Astrophysical Journal, Volume 693, Issue 1, pp. 236-249 (2009). (ApJ Homepage)
Publication Date:
03/2009
Origin:
IOP
ApJ Keywords:
accretion, accretion disks, novae, cataclysmic variables, stars: individual: V592 Cas
DOI:
10.1088/0004-637X/693/1/236
Bibliographic Code:
2009ApJ...693..236H

Abstract

We present the ultraviolet-optical-infrared spectral energy distribution of the low inclination novalike cataclysmic variable (CV) V592 Cassiopeiae, including new mid-infrared observations from 3.5 to 24 μm obtained with the Spitzer Space Telescope. At wavelengths shortward of 8 μm, the spectral energy distribution of V592 Cas is dominated by the steady state accretion disk, but there is flux density in excess of the summed stellar components and accretion disk at longer wavelengths. Reproducing the observed spectral energy distribution from ultraviolet to mid-infrared wavelengths can be accomplished by including a circumbinary disk composed of cool dust, with a maximum inner edge temperature of ≈500 K. The total mass of circumbinary dust in V592 Cas (~1021 g) is similar to that found from recent studies of infrared excess in magnetic CVs, and is too small to have a significant effect on the long-term secular evolution of the cataclysmic variable. The existence of circumbinary dust in V592 Cas is possibly linked to the presence of a wind outflow in this system, which can provide the necessary raw materials to replenish the circumbinary disk on relatively short timescales, and/or could be a remnant from the common envelope phase early in the formation history of the system.
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