Asymptotic models of accretion disc boundary layers

Details Asymptotic models of accretion disc boundary layers Asymptotic models of accretion disc boundary layers

Jan 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995mnras.272...71r&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 272, Issue 1, pp. 71-79.

Astronomy and Astrophysics

Astronomy

22

Accretion, Accretion Discs-Binaries, Close-White Dwarfs

Scientific paper

Accretion disc boundary layer models are constructed with the help of the matched asymptotic expansion (MAE) method. Using an improved, double inner expansion technique, we demonstrate the existence, depending on the nature of the assumed boundary conditions, of both cool and hot boundary layer solutions. Namely, we find that models where the radiative flux is fixed at the inner boundary yield hot boundary layers that radiate outwards, while models where the temperature is fixed at the inner boundary yield cool boundary layers that radiate into the star. The effects of boundary layer energy input into the star are examined, using an approximate radiative transfer calculation appropriate to the case of accreting T Tauri stars. We find that cool and hot boundary layers are observationally indistinguishable in this case. It is argued that differences between the two types of solutions may be apparent in slowly rotating accretion white dwarfs.

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