Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1977
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977apj...217..530w&link_type=abstract
Astrophysical Journal, Part 1, vol. 217, Oct. 15, 1977, p. 530-536.
Astronomy and Astrophysics
Astrophysics
23
Binary Stars, Dwarf Stars, Mass Transfer, Novae, Stellar Mass Ejection, Giant Stars, Main Sequence Stars, Mass Flow Rate, Radiative Transfer, Roche Limit, Stellar Models
Scientific paper
The stability of mass transfer from semidetached secondaries in binary systems has been studied by incorporating some improvements on the previous calculations of Bath (1975), including a revised outer boundary condition, convective energy transport, and a line-of-centers gravitational potential. Main-sequence secondaries with effective temperatures of at least 5000 K (masses of at least 0.8 solar mass) are found to transfer mass in pulses, while cooler (less massive) secondaries transfer mass continuously. The calculations suggest that if dwarf nova outbursts are caused by a variable mass-transfer rate from the secondary, then the outbursts may occur only at intervals in the lifetime of a binary system, long quiescent periods existing between the dwarf nova phases. In view of the continuous mass outflow found in the less massive secondaries, a disk instability is required to explain dwarf nova outbursts in systems containing such secondaries. A lobe-filling giant with parameters similar to those of the secondary in the recurrent nova T CrB is found to transfer mass continuously.
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