By Henri M. J. Boffin, Giovanni Carraro, Giacomo Beccari
The life of blue straggler stars, which look more youthful, warmer, and extra enormous than their siblings, is at odds with an easy photo of stellar evolution. Such stars must have exhausted their nuclear gasoline and advanced in the past to develop into cooling white dwarfs. they're came upon to exist in globular clusters, open clusters, dwarf spheroidal galaxies of the neighborhood workforce, OB institutions and as box stars.
This booklet summarises the numerous advances in observational and theoretical paintings devoted to blue straggler stars. conscientiously edited prolonged contributions through famous specialists within the box hide the entire suitable facets of blue straggler stars learn: Observations of blue straggler stars of their a variety of environments; Binary stars and formation channels; Dynamics of globular clusters; Interpretation of observational facts and comparability with types. The e-book additionally bargains an introductory bankruptcy on stellar evolution written via the editors of the book.
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Additional info for Ecology of Blue Straggler Stars
Interestingly, such a dynamical origin would require the encounter to have been more recent than the short tidal circularisation timescale at these small orbital periods. 3 Secondary-Star Mass Distribution Only two of the blue-straggler binaries are double-lined; for the other 14 our information about the secondary stars derives only from the mass functions of single-lined orbital solutions. Given the unknown inclination, and indeed the poorly known masses of the blue straggler primary stars, standard statistical techniques (Mazeh and Goldberg 1992) must be used to determine the mass distribution of the secondary stars of these blue-straggler binaries.
In this case, therefore, the mixing involves extremely profound regions of the star ( 75 % of the structure) and generates chemical signatures that differ form those characterising the other two dredge-ups, such as an increase of the abundance of carbon at the surface. During the entire duration of the AGB phase, the stars may be affected by phenomena of substantial mass loss. This is due to the fact that the envelope of these 12 G. Beccari and G. Carraro stars is expanded and cold as ever during the other phases of evolution: therefore the formation of layers of molecules and dust becomes possible, layers which are then removed as stellar wind by the effect of radiation pressure.
Xin et al. (2011) have shown that BSSs can be numerous enough to contribute 10 % to the integrated light of star clusters at short wavelengths (see also Chap. 14 in this volume). References Ahumada, J. : A&A 463, 789 (2007) Arp, H. , Baum, W. , Sandage, A. : AJ 58, 4 (1953) Arp, H. : ApJ 136, 51 (1962) Arp, H. , Hartwick, F. D. : ApJ 167, 499 (1971) Bailyn, C. : ARA&A 33, 133 (1995) Bond, H. , McConnell, D. : ApJ 165, 51, (1971) Bond, H. : PASP 83, 6388, (1971) Burbidge, E. , Sandage, A. : ApJ 128, 174, (1958) Cannon, R.
Ecology of Blue Straggler Stars by Henri M. J. Boffin, Giovanni Carraro, Giacomo Beccari