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Theory and Observations of Accretion Disc Spectra

Published online by Cambridge University Press:  12 April 2016

S.K. Mayo
Affiliation:
Royal Greenwich Observatory, Hailsham, U.K. Institute of Astronomy, Cambridge, U.K.
D.T. Wickramasinghe
Affiliation:
Institute of Astronomy, Cambridge, U.K. Department of Applied Mathematics, Australian National University, Canberra, Australia
J.A.J. Whelan
Affiliation:
Institute of Astronomy, Cambridge, U.K.

Extract

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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.

Type
Colloquium Session VI
Copyright
Copyright © The University of Rochester 1979

References

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Mayo, S.K., Wickramasinghe, D.T. and Whelan, J.A.J. 1978. IAU Coll. 46, Hamilton, New Zealand.Google Scholar
Mayo, S.K., Wickramasinghe, D.T. and Whelan, J.A.J. 1979. Submitted to M.N.R.A.S.Google Scholar
Schwarzenberg-Czerny, A. and Rózyczka, M. 1977. Acta Astr., 27, 429.Google Scholar
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