On the origin of hot subdwarfs in globular clusters

Details On the origin of hot subdwarfs in globular clusters On the origin of hot subdwarfs in globular clusters

Dec 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...347l..21b&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 347, Dec. 1, 1989, p. L21-L24.

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38

B Stars, Binary Stars, Blue Stars, Globular Clusters, Subdwarf Stars, Computational Astrophysics, Stellar Evolution, Stellar Luminosity, Stellar Mass, White Dwarf Stars

Scientific paper

Recent observations have unveiled the existence of a large population of subdwarf B stars in several globular clusters. It is suggested that these stars are the consequences of mergers of low-mass helium white dwarf pairs that were formed from primordial main-sequence binaries. Such mergers may be hastened by close encounters between the precursor double degenerate pairs and other cluster members; these encounters serve to harden the binary sufficiently that gravitational wave radiation will force contact in much less than a Hubble time. The presence of mergers caused by encounters may explain the variations in central concentration and numbers of these stars in different clusters.

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