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Frequency of Be and Ae stars in spectroscopic binaries
Astrophysics and Space Science, 1986The frequency of Be and Ae stars in spectroscopic binaries and Algol binaries is examined based on the available catalogue data, and compared with that of stars in theBright Star Catalogue. It is shown that in binary systems Be and Ae stars reveal different statistical behaviours. The frequency of Be stars in spectroscopic binaries shows a notable peak
Tomokazu Kogure, Masakazu Suzuki
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On the reflection effect in spectroscopic binary stars
Vistas in Astronomy, 1970Abstract It is shown that both spectroscopic observations and observations of reddening during eclipses of close binary stars indicate the existence of “hot spot” conditions over an area of a “reflecting” star that cannot be explained by a simple geometrical model of reflection.
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Research in Astronomy and Astrophysics, 2019
About 786.4 thousand stars were observed by LAMOST twice or more during the first stage of its spectroscopic survey. The radial velocity differences for about 256 thousand targets are larger than 10 km s−1 and they are possible spectroscopic binary or ...
S. Qian +9 more
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About 786.4 thousand stars were observed by LAMOST twice or more during the first stage of its spectroscopic survey. The radial velocity differences for about 256 thousand targets are larger than 10 km s−1 and they are possible spectroscopic binary or ...
S. Qian +9 more
semanticscholar +1 more source
Statistical study of Am stars in spectroscopic binary systems
Astrophysics and Space Science, 1978Using the Am components in spectroscopic binaries, the region of metallicism in the (logm, logR) diagram is statistically discussed. The metallic-line characteristics appear in a slightly evolved stage near the Main Sequence within a belt characterized by logg=3.8–4.2, for which the radiiR/R ⊙=1.5–2.7.
Masatoshi Kitamura, Masayuki Kondo
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A spectroscopic study of the binary Be star Phi Persei
Publications of the Astronomical Society of the Pacific, 1981High-dispersion high signal-to-noise ratio spectrograms of Phi Per have been obtained. The radial velocities of various spectral features have been measured and an orbit solution obtained. The Phi Persei system is found to consist of a 21 solar mass star, whose V sin i is 450 km/s, and a 3.4 solar mass secondary. The secondary is peculiar in that He II
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Determination of the mass-ratio distribution, II: Double-lined spectroscopic binary stars
, 1992S. J. Hogeveen
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Errata in second catalogue of spectroscopic binary stars
Lick Observatory Bulletins, 1911openaire +2 more sources
Synchronization in early-type spectroscopic binary stars
1984GIURICIN G. +2 more
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