Mirror eclipses in the cataclysmic variable IP Peg
arXiv:astro-ph/0106181 · doi:10.1046/j.1365-8711.2001.04744.x
Abstract
We present time resolved K-band infrared spectra of the dwarf nova (DN) IP Peg in early quiescence. The Brackett-gamma and HeI lines in our data show hitherto unseen behaviour, which we term a mirror eclipse, and interpret as an eclipse of the secondary star by an optically thin accretion disc. Mirror eclipses are a direct probe of the structure and physical conditions of accretion discs. For example, on assuming the relevant level populations to be in LTE, we constrain the temperature and density of the optically thin material causing the mirror eclipse to be 10,000 < T < 20,000 K and ρ~10^-11 g/cm^3 respectively. In order to match our data we find that at least the outermost 20% of the disc (in radius) must be entirely optically thin. Implications for time-dependant disc models are examined.
10 pages, 8 figures, to appear in monthly notices (accepted) (replaced with references)
References in corpus (1)
Cited by in corpus (11)
- Physical properties of IP Pegasi: an eclipsing dwarf nova with an unusually cool white dwarf
- Excess mid-IR emission in Cataclysmic Variables
- V1460 Her: A fast spinning white dwarf accreting from an evolved donor star
- Observational Constraints Upon Cool Disk Material in Quiescent Black Hole Binaries
- Accretion-disc model spectra for dwarf-nova stars
- The masses, radii and luminosities of the components of U Geminorum
- A multicolor near-infrared study of the dwarf nova IP Peg
- The Patchy Accretion Disc in HT Cassiopeiae
- Outburst Photometry of the Eclipsing Dwarf Nova GY Cancri
- 1RXH J082623.6-505741: a new long-period cataclysmic variable with an evolved donor and a low mass transfer rate
- Spectra of accretion discs around white dwarfs