Astronomy and Astrophysics – Astronomy
Scientific paper
Oct 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...273l..81p&link_type=abstract
Astrophysical Journal, Part 2 - Letters to the Editor (ISSN 0004-637X), vol. 273, Oct. 15, 1983, p. L81-L84.
Astronomy and Astrophysics
Astronomy
33
Binary Stars, Black Holes (Astronomy), Magellanic Clouds, Stellar Mass, X Ray Sources, B Stars, Mass To Light Ratios, Stellar Evolution, Stellar Mass Accretion
Scientific paper
The lower mass limit for LMC X-3 is obtained taking into account the absence of X-ray eclipses and not allowing the B star to exceed its Roche lobe radius. The mass limit depends on the B star radius. For a plausible value of 6 solar radii, the minimum mass of the X-ray component is 10 solar masses. This result does not depend on the structure or evolutionary status of either component. The upper mass limit for the B star is estimated to be 6.6 solar masses, almost independent of its evolutionary status. This implies that the optical star is less massive than the X-ray component and that the Roche lobe overflow may be stable. If the B star is on the main sequence, then its expansion due to nuclear evolution may give rise to the mass transfer rate of 10 to the -7th solar mass per year and the total accretion luminosity of 10 to the 39th ergs/s. Reflection effect due to X-ray heating as well as ellipsoidal light variations are expected to be seen in the light curve of this system.
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