The old galactic cluster NGC 188 and the origin of the W Ursae Majoris-type contact binaries

Details The old galactic cluster NGC 188 and the origin of the W Ursae Majoris-type contact binaries The old galactic cluster NGC 188 and the origin of the W Ursae Majoris-type contact binaries

Jul 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...294..207b&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 294, July 1, 1985, p. 207-215. Research supported by the Langley-Abbot Foun

Astronomy and Astrophysics

Astrophysics

24

Binary Stars, Galactic Clusters, Stellar Evolution, Stellar Spectrophotometry, Variable Stars, Absorption Spectra, Angular Momentum, Color-Magnitude Diagram, Light Curve, Open Clusters, Radial Velocity, Stellar Winds

Scientific paper

Spectroscopic observations of the four faint, short-period light variables EP Cep, EQ Cep, ER Cep, and ES Cep confirm that they are W UMa-type, or contact, binaries. The binaries EP Cep and ES Cep are members of the old open cluster NGC 188 (age about 5-10 x 10 to the 9th yr) by a radial-velocity criterion; all four are associated with the cluster by their position in space and in its color-magnitude diagram. Combined with the light curves of the variables, the inferred component radial velocities reveal spectroscopic mass ratios that characterize these binaries as "W-type' systems that are physically similar to those in the field. The high spatial incidence of these systems in a cluster of such great age suggests that these stars have evolved into the contact configuration from detached or semidetached progenitors that lose orbital angular momentum, perhaps through magnetic braking in stellar winds. The W UMa-type binaries may coalesce and form the rapidly rotating yellow giants, the FK Comae stars.

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