Duplicity of late B-type stars

Details Duplicity of late B-type stars Duplicity of late B-type stars

Jun 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...222..556w&link_type=abstract

Astrophysical Journal, Part 1, vol. 222, June 1, 1978, p. 556-569.

Astronomy and Astrophysics

Astrophysics

55

B Stars, Binary Stars, Early Stars, Stellar Mass, Stellar Spectrophotometry, A Stars, Periodic Variations, Radial Velocity, Stellar Rotation, Synchronism, Tables (Data)

Scientific paper

High-dispersion spectroscopic observations of 83 stars are used to determine the binary characteristics of late B-type stars. For a random sample of such objects, including peculiar as well as normal stars, the frequency of binaries with mass ratios m2/m sub 1 greater than 0.1 and orbital periods less than 100 days is estimated to be about 24%, and the frequency of binaries decreases with decreasing m2/m sub 1. In both respects, the late B-type stars are similar to early B-, late A-, and solar-type stars. For the majority of stars with an orbital period greater than 4 days, the observed rotational velocity exceeds the value that corresponds to synchronism of rotation and revolution, but the ratio of the observed to the synchronous rotational velocity seldom exceeds a factor of 2 even for periods as long as 15 days. An additional 20% of the stars surveyed exhibit low amplitude-velocity variations that, if due to orbital motion, correspond to m2 m1 less than 0.1. The most likely explanation is that these systems are close binary remnants that have already passed through the mass-transfer phase, with the present secondary being a white dwarf.

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