Computer Science – Numerical Analysis
Scientific paper
Dec 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994pasj...46..613u&link_type=abstract
PASJ: Publications of the Astronomical Society of Japan (ISSN 0004-6264), vol. 46, no. 6, p. 613-619
Computer Science
Numerical Analysis
9
Astronomical Models, Binary Stars, Gravity Anomalies, Mass Transfer, Starspots, Stellar Envelopes, Stellar Gravitation, Stellar Mass, Stellar Physics, Bernoulli Theorem, Brightness Distribution, Enthalpy, Kinetic Energy, Mathematical Models, Numerical Analysis, Photosphere, Radiative Transfer, Stellar Winds
Scientific paper
The anomalous high correlation of the surface brightness to the surface gravity on the secondary of a semi-detached system is interpreted by the enthalpy transport associated with the mass-outflow from the secondary filling the Roche lobe. Quasi-radial flow in the subadiabatic stellar envelope from the deep interior is the cause of darkening. The speed of the flow, however, is essentially given by the condition of the subsonic-supersonic transition through the region in the neighborhood of the L1 Lagrangian point. The consequence of the mass-outflow is the formation of star spots at low gravity regions on the front and back sides of the secondary towards the primary. These star spots show photospheric depressions caused by lower opacities, like the Wilson depression in sunspots. The anomalous gravity darkening can be considered as being a manifestation of the internal structure of the secondary of a semi-detached binary system, measuring the subadiabaticity in the interior through which the flow has traversed. Stars showing strong and less strong gravity darkening are stars of relatively high and low temperatures having radiative and convective envelopes, respectively. The mass-loss rate, which accounts for anomalous gravity darkening, is estimated to be approximately 10-6 solar mass/y.
Kiguchi Masayoshi
Kitamura Masatoshi
Unno Wasaburo
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