The Quiescent Accretion Disk in IP Peg at Near-Infrared Wavelengths

Details The Quiescent Accretion Disk in IP Peg at Near-Infrared Wavelengths The Quiescent Accretion Disk in IP Peg at Near-Infrared Wavelengths

1999-03-22

arxiv.org/abs/astro-ph/9903328v3

Astronomy and Astrophysics

Astrophysics

Corrected minor typos, 7/99. Paper in press, will appear in September 20, 1999 issue of the ApJ. Accepted for publication in T

Scientific paper

10.1086/307713

We present near-infrared, H-band (1.45-1.85 microns) observations of the eclipsing dwarf nova, IP Peg, in quiescence. The light curves are composed of ellipsoidal variations from the late-type secondary star and emission from the accretion disk and the bright spot. The light curves have two eclipses: a primary eclipse of the accretion disk and the bright spot by the companion star, and a secondary eclipse of the companion star by the disk. The ellipsoidal variations of the secondary star were modeled and subtracted from the data. The resulting light curve shows a pronounced double-hump variation. The double-hump profile resembles those seen in the light curves of WZ Sge and AL Com and likely originates in the accretion disk. The primary eclipse was modeled using maximum entropy disk mapping techniques. The accretion disk has a flat intensity distribution and a cool brightness temperature (Tbr=3000 K) in the near-infrared. Superimposed on the face of the disk is the bright spot (Tbr=10,000 K); the position of the bright spot is different from the observed range of visible bright spot positions. The near-infrared accretion disk flux is dominated by optically thin emission. The secondary eclipse indicates the presence of some occulting medium in the disk, but the eclipse depth is too shallow to be caused by a fully opaque accretion disk.

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