Evolution of the subdwarf O eclipsing binary LB 3459

Details Evolution of the subdwarf O eclipsing binary LB 3459 Evolution of the subdwarf O eclipsing binary LB 3459

Jun 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982esasp.176..343k&link_type=abstract

In ESA 3rd European IUE Conf. p 343-348 (SEE N83-11889 02-88)

Computer Science

Eclipsing Binary Stars, Magellanic Clouds, Stellar Evolution, Subdwarf Stars, Abundance, Chemical Composition, Helium, Light Curve, Photosphere, Stellar Gravitation, Stellar Mass, Stellar Structure, Stellar Temperature

Scientific paper

Ground based and IUE spectra were used in an NLTE analysis of the LB 3459 primary. Effective temperature = 40,000 K (+3000, -2000), log g = 5.3 + or - 0.2, with helium abundance = 0.3% (+0.2, -0.1) by number. The binary seems to be the result of mass exchange during the first giant phase. The primary is thought to have a mass of 0.3M and consists of a hydrogen shell and degenerate helium core. Diffusion is suggested as the cause of helium depletion in the photosphere. From light curve synthesis, a secondary effective temperature of 8500 + or 2000 K is suggested. The secondary mass is 0.04M and the radius is 0.09R. This is close to a degenerate configuration of solar composition.

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