Astronomy and Astrophysics – Astrophysics
Scientific paper
Sep 1975
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975ap%26ss..36..407w&link_type=abstract
Astrophysics and Space Science, vol. 36, Sept. 1975, p. 407-426. Research supported by the University of Wisconsin.
Astronomy and Astrophysics
Astrophysics
2
Astronomical Models, Eclipsing Binary Stars, Emission Spectra, Lagrangian Equilibrium Points, Stellar Spectra, Gas Density, Gas Heating, H Gamma Line, Light Curve, Novae, Ring Structures, Stellar Envelopes, Stellar Mass Ejection, Three Body Problem, Velocity Distribution
Scientific paper
It is proposed that the observed double-component emission lines in the spectrum of RW Tauri originate at the triangular Lagrangian points, L4 and L5, of the restricted three-body problem. The light curves of many close binary systems show absorption dips at plus or minus 60 deg of the primary (and sometimes also the secondary) minimum, indicating appreciable accumulation of matter at these points. The orbital velocity of L4 and L5 is derived as a function of period and the masses of the component stars. This equation is an independent relationship for determining the two stellar masses and reproduces Struve's (1946) empirical finding that the cube of the velocity is inversely proportional to the period. The observed emission-line velocity is consistently higher than the calculated orbital velocity of L4 and L5. This is due to the serious erosion of the low-velocity sides of the emission components by the stellar and shell absorption lines. There is observational evidence which indicates that the intermittent high-velocity radial ejection of matter is a mode of mass loss from the secondary. The energy of mass motion from this ejection is sufficient, and may be responsible, for heating the gas at L4 and L5. The ionizing radiation emitted by the primaries of Algol systems is shown to be many orders of magnitude below that required by the observed strength of the emission lines.
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