Astronomy and Astrophysics – Astrophysics
Scientific paper
Sep 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986japa....7..195g&link_type=abstract
Journal of Astrophysics and Astronomy (ISSN 0250-6335), vol. 7, Sept. 1986, p. 195-223. SERC-supported research.
Astronomy and Astrophysics
Astrophysics
66
Binary Stars, Stellar Mass, Stellar Spectra, Giant Stars, Late Stars, Main Sequence Stars, Radial Velocity, Stellar Luminosity, Stellar Orbits, Stellar Rotation, Stellar Spectrophotometry
Scientific paper
Composite-spectrum binary stars generally consist of a late-type giant and a main-sequence star of type A or B. Their spectra are therefore rather confusing; but by a technique of digital subtraction of the spectra of appropriate single late-type giants, composite spectra can be split into their individual components. In favorable cases, the radial velocities of both components can be measured and the mass ratio determined. The procedures are illustrated by reference to HR 6902, a fifth-magnitude composite-spectrum binary. Its components are shown to have spectral types of G9 II and B8 V, with a mass ratio of 1.31, and its orbit is determined. There is some evidence that the system shows eclipses. If it does, the masses of the components are 3.9 and 3.0 solar masses respectively, and HR 6902 becomes the sixth known member of the important class of Zeta Aur binaries.
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