Statistics – Computation
Scientific paper
Sep 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985mnras.216...37p&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 216, Sept. 1, 1985, p. 37-52.
Statistics
Computation
51
Cataclysmic Variables, Convection, Stellar Evolution, Stellar Mass Accretion, Computational Astrophysics, Stellar Luminosity, Stellar Models, Stellar Temperature
Scientific paper
The authors perform evolutionary calculations of a 0.2 M_sun; fully convective star accreting matter at a rate M, ranging from 10-1M_sun;yr-1 to 10-10M_sun;yr-1, until the amount of mass accumulated reaches 2.5×10-3M_sun;. They assume the star to gain energy through accretion at a rate αGMM/R, with α ranging from 0.001 to 0.5. They find that the final models may be divided into three main groups according to their response to accretion. For low Mor low α (Group A) the star remains fully convective and contracts upon accretion. For high α and high M(Group C) the star expands rapidly and in some cases becomes dynamically unstable. In the intermediate range of Mand α (Group B) the outer radius of the star grows, although the interior contracts slowly.
Livio Mario
Prialnik Dina
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