75 PEGASI, A VERY-SHORT-PERIOD EXTREME MASS RATIO BINARY

The bright star 75 Peg has long been known to be a spectroscopie binary. The orbital parameters are presented here for the first time, and include the very short period of 0ḍ5021035. The system has one of the most extreme values of mass ratio known. The most direct interpretation of the available sp...

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Bibliographic Details
Published inPublications of the Astronomical Society of the Pacific Vol. 97; no. 589; pp. 280 - 284
Main Authors HUBE, DOUGLAS P., GULLIVER, AUSTIN F.
Format Journal Article
LanguageEnglish
Published Chicago, IL The Astronomical Society of the Pacific 01.03.1985
University of Chicago Press
Subjects
Astronomy
Binary and multiple stars
Earth, ocean, space
Exact sciences and technology
Main sequence stars
Mass ratio
Mass spectroscopy
Observatories
Orbital elements
Orbital velocity
Radial velocity
Rotation
Spectroscopic binaries. Close binaries
Stars
Stellar radii
Data table
Radial velocity
Short period variable star
Spectroscopic binary
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Summary:The bright star 75 Peg has long been known to be a spectroscopie binary. The orbital parameters are presented here for the first time, and include the very short period of 0ḍ5021035. The system has one of the most extreme values of mass ratio known. The most direct interpretation of the available spectroscopie observations leads to the conclusion that the primary fills, or is very close to filling, its critical Roche lobe, and will begin to lose mass to its companion before leaving the main sequence.
Bibliography:ObjectType-Article-2
SourceType-Scholarly Journals-1
ObjectType-Feature-1
content type line 23
ISSN:0004-6280
1538-3873
DOI:10.1086/131530