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• W3048532054 abstract "The binaries-in-clusters program of the Rotbney Astrophysical Observatory has targeted eclipsing binaries in galactic star clusters since 1975. The program uses a boot strap method: fundamental star data are obtained from light curve analysis and these data then elucidate the properties of the cluster environment, such as the distance, reddening, and, through isochrone fittings, information about the age and evolution of both binary components and the cluster as a whole. Here we discuss its current status and the increasingly important role of all-cluster direct and spectroscopic imaging. It is now clear that the role played by binary stars is central to our understanding of clusters (cf. Hut et al. 1992). The evaporation of the high energy tail from a cluster leads to a more strongly bound core and to its eventual collapse, and stellar collisions provide the evaporants. Since binary star encounters are more probable than single star encounters by a factor of order a/R (where a and R are the semi-major axis and stellar radius, respectively), binaries are an important determinant of cluster evolution. NGC 5466 is a low-density globular cluster, at least 48 stars of which are blue stragglers (Nemec & Harris 1987), which may be primordial objects since they are somewhat more centrally concentrated than subgiants. If the BSs are indeed merged binaries, were they formed through collisions or through magnetic braking? Masses are needed to decide the issue: are the components more massive than the turn-off mass or not? If the blue straggler masses are consistent with those expected from primordial binary evolution scenarios, probably they formed through magnetic braking, and the numbers of blue stragglers may be indicative of the primordial binary population. The existence of three short-period eclipsing systems among the BSs in this ancient ('t -18 Gy) cluster (Nemec & Harris 1987) offers strong support to the late evolution of such close binaries, either by merger through angular momentum loss or through repeated collisions in the cluster core, or both. Detailed analysis (Kallrath, Milone & Stagg 1992) of the Mateo et al. (1990) CCD BV light curves indicated a slight preference for a detached, transit solution over either semi-detached or detached, occultation solution for NH31; both NH19 and NH30 are overcontact A-type W UMa systems, very close to their outer lobes, with contact parameter, f - 0.94. In each case the primary star is itself a blue-straggler (Milone, Stagg & Kallrath 1992), requiring multiple mergers (Leonard & Linnell 1992) to sustain the merger scenario as the origin of the BSs. Yet, the cluster is so sparse and the velocity dispersion so low in the core that the average time between even wide collisions (lOx orbital separation) is 1013 y" @default.
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• W3048532054 date "1994-01-01" @default.
• W3048532054 modified "2023-10-18" @default.
• W3048532054 title "TIlE BINARIES·IN·CLUSTERS PROGRAM IN TIlE AGE OF IMAGING" @default.
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