The Accretion Disk and White Dwarf in the U Geminorum type Dwarf Novae UZ Serpentis and SS Aurigae during Quiescence

  • Lake J
  • Sion E
10Citations
Citations of this article
5Readers
Mendeley users who have this article in their library.

Abstract

We have carried out high-gravity model atmosphere and accretion disk synthetic spectral fits for the U Geminorum type dwarf novae during quiescence. For UZ Ser, we find that the far-UV spectrum is best fitted with a log g = 8, Teff = 27,000 K photosphere with abundances near solar. The best-fit accretion disk model for UZ Ser has Mwd = 1.0 M⊙, disk inclination i = 75°, and M = 10-9 M⊙ yr-1. For SS Aur, the best-fit model photosphere has Teff = 30,000K, log g = 8, and solar composition abundances, while the best-fit accretion disk model has Mwd = 1.0 M⊙, i = 41°, and Ṁ = 10-10 M⊙ yr-1. These accretion rates are discussed in connection with the critical accretion rates predicted by the disk instability theory. Whether a white dwarf or a disk accounts for the far-UV spectra, they must be quite hot. If indeed the white dwarf dominates the far-UV light, then UZ Ser and SS Aur add two important temperatures in support of the conclusion that the accreting white dwarfs above the period gap are a factor of 1.5-2 times hotter than the accreting cataclysmic variable degenerates in systems below the period gap.

Cite

CITATION STYLE

APA

Lake, J., & Sion, E. M. (2001). The Accretion Disk and White Dwarf in the U Geminorum type Dwarf Novae UZ Serpentis and SS Aurigae during Quiescence. The Astronomical Journal, 122(3), 1632–1635. https://doi.org/10.1086/322096

Register to see more suggestions

Mendeley helps you to discover research relevant for your work.

Already have an account?

Save time finding and organizing research with Mendeley

Sign up for free