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Theory and Observations of Accretion Disc Spectra

  • S.K. Mayo (a1) (a2), D.T. Wickramasinghe (a2) (a3) and J.A.J. Whelan (a2)

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Theoretical continua (3000 ≲ λ (Å) ≲ 20000), UBV colours and Balmer absorption line profiles (Hα – Hδ) have been computed for the optically thick parts of steady-state accretion discs around white dwarfs as a function of mass flow rate, mass of white dwarf and inclination angle. The uncertainties due to disc z-structure and outer radius and viscosity are considered.

The theoretical results for continua and UBV colours are compared with the theoretical results of Schwarzenberg-Czerny and Rózyczka (1977) and Herter et al. (1979) and with results obtained using black bodies instead of stellar atmospheres (e.g. Lynden-Bell 1969). Where models can be directly compared the quantitative agreement is good.

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References

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Herter, T., Lacasse, M.G., Wesemael, F. and Winget, D.E. 1979. Astrophys. J.Suppl., 39, 513.
Lynden-Bell, D. 1969. Nature, 233, 690.
Mayo, S.K. 1979. Ph.D. Thesis in preparation. University of Cambridge.
Mayo, S.K., Wickramasinghe, D.T. and Whelan, J.A.J. 1978. IAU Coll. 46, Hamilton, New Zealand.
Mayo, S.K., Wickramasinghe, D.T. and Whelan, J.A.J. 1979. Submitted to M.N.R.A.S.
Schwarzenberg-Czerny, A. and Rózyczka, M. 1977. Acta Astr., 27, 429.
Warner, B. 1976. Observatory, 96, 49.

Theory and Observations of Accretion Disc Spectra

  • S.K. Mayo (a1) (a2), D.T. Wickramasinghe (a2) (a3) and J.A.J. Whelan (a2)

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