Mass loss in semi-detached binaries

Details Mass loss in semi-detached binaries Mass loss in semi-detached binaries

Feb 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984ap%26ss..99..355a&link_type=abstract

(International Astronomical Union, Colloquium on Double Stars, Physical Properties and Generic Relations, 80th, Bandung, Indones

Astronomy and Astrophysics

Astrophysics

6

Binary Stars, Hertzsprung-Russell Diagram, Main Sequence Stars, Stellar Evolution, Stellar Mass, Abundance, Chemical Composition, Helium, Molecular Weight, Nuclear Fusion

Scientific paper

Pre-main-sequence contracting objects, post-main-sequence expanding stars and mass-losing components of semi-detached systems all occupy more or less the same region in the conventional H-R diagram. A transformation is made to variables Δ (log L) and Δ (log Te), where Δ is the difference between the observed quantity, log L or log Te, and the value of that quantity which a star of the same mass would have on the empirical main sequence. It is demonstrated that a plot between the new variables clearly separates the mass-losing stars from other objects. This is essentially an effect of the increasing abundance of helium relative to hydrogen.

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