Statistics – Computation
Scientific paper
Nov 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...239..163s&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 239, no. 1-2, Nov. 1990, p. 163-172.
Statistics
Computation
9
Cataclysmic Variables, Computational Astrophysics, Red Dwarf Stars, Stellar Luminosity, Accretion Disks, Astronomical Models, Energy Transfer, Stellar Mass Accretion
Scientific paper
The instability models of illuminated secondary components in cataclysmic variables (CV) by Osaki (1985) and of soft X-rays transients by Hameury et al. (1986) are discussed and compared. It is shown that only the isothermal approximation of the outer layer of the envelope near the Lagrangian point L1 gives the correct value of the mass density rho L1 at this point. It is found that the effect of illumination of the secondary in CVs by the UV and X-ray fluxes does not generate the mass transfer instability through the L1 point. The fact that the L1 point in CVs is not directly illuminated by UV and X-rays, but is shielded by the accretion disk is being taken into account. Therefore, a meridional circulation as energy transport mechanism (Kippenhahn and Thomas, 1979) is considered. It is demonstrated that only a small region near the L1 point, where convection is nonadiabatic, is important for the mass transfer modulations.
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