Volume 433, Number 3, April III 2005
|Page(s)||1085 - 1095|
|Section||Stellar structure and evolution|
|Published online||29 March 2005|
HST/FOS time-resolved spectral mapping of IP Pegasi at the end of an outburst
Departamento de Física, Universidade Federal de Santa Catarina, Trindade, 88040-900, Florianópolis, SC, Brazil e-mail: firstname.lastname@example.org
2 School of Physics and Astronomy, University of St. Andrews, KY16 9SS, Scotland, UK
Accepted: 21 December 2004
We report an eclipse mapping analysis of time-resolved ultraviolet spectroscopy covering three eclipses of the dwarf nova IP Pegasi on the late decline of the 1993 May outburst. The eclipse maps of the first run show evidence of one spiral arm, suggesting that spiral structures may still be present in the accretion disc 9 days after the onset of the outburst. In the spatially resolved spectra the most prominent lines appear in emission at any radius, being stronger in the inner disc regions. The spectrum of the gas stream is clearly distinct from the disc spectrum in the intermediate and outer disc regions, suggesting the occurrence of gas stream overflow. The full width half maximum of C IV is approximately constant with radius, in contrast to the expected law for a gas in Keplerian orbits. This line probably originates in a vertically extended region (chromosphere + disc wind). The uneclipsed component contributes ~4% of the flux in C IV in the first run, and becomes negligible in the remaining runs. We fit stellar atmosphere models to the spatially resolved spectra. The radial run of the disc color temperature for the three runs is flatter than the expected law for steady-state optically thick discs models, with K in the inner regions and K in the outer disc regions. The solid angles that result from the fits are smaller than expected from the parameters of the system. The radial run of the solid angle suggests that the disc is flared in outburst, and decreases in thickness toward the end of the outburst.
Key words: stars: individual: IP Peg / stars: binaries: eclipsing / methods: data analysis
© ESO, 2005
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