Changes in the structure of the accretion disc of EX Draconis through the outburst cycle
| Autor: | M. S. Catalán, Raymundo Baptista |
|---|---|
| Rok vydání: | 2001 |
| Předmět: |
Physics
Brightness Astrophysics::High Energy Astrophysical Phenomena Astrophysics (astro-ph) FOS: Physical sciences Flux Astronomy and Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics Astrophysics Instability Photometry (optics) Space and Planetary Science Brightness temperature Astrophysics::Solar and Stellar Astrophysics Roche lobe Astrophysics::Earth and Planetary Astrophysics Dwarf nova Astrophysics::Galaxy Astrophysics Eclipse |
| Zdroj: | Monthly Notices of the Royal Astronomical Society. 324:599-611 |
| ISSN: | 1365-2966 0035-8711 |
| Popis: | (Abridged) We report on the analysis of high-speed photometry of the dwarf nova EX Dra through its outburst cycle with eclipse mapping techniques. The eclipse maps show evidence of the formation of a one-armed spiral structure in the disc at the early stages of the outburst and reveal how the disc expands during the rise until it fills most of the primary Roche lobe at maximum light. The eclipse maps also suggest the presence of an inward and an outward-moving heating wave during the rise and an inward-moving cooling wave in the decline. Our results suggest a systematic deceleration of both the heating and the cooling waves as they travel across the disc, in agreement with predictions of the disc instability model. The analysis of the brightness temperature profiles indicates that most of the disc appears to be in steady-state during quiescence and at outburst maximum, but not during the intermediate stages. As a general trend, the mass accretion rate in the outer regions is larger than in the inner disc on the rising branch, while the opposite holds during the decline branch. We estimate a mass accretion rate of Mdot= 10^{-8} Msun/yr at outburst maximum and Mdot= 10^{-9.1} Msun/yr in quiescence. The brightness temperature profile in quiescence also suggests that the viscosity parameter is high at this stage which favours the mass-transfer instability model. The uneclipsed light has a steady component, understood in terms of emission from the red secondary star, and a variable component that is proportional to the out of eclipse flux and corresponds to about 3 per cent of the total brightness of the system. The variable component is interpreted as arising in a disc wind. To appear in Mon. Not. R. Ast. Soc., 14 pages, 9 figures, coded with MNRAS latex style |
| Databáze: | OpenAIRE |
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