Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...347..998e&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 347, Dec. 15, 1989, p. 998-1011. Research supported by the Canadian Institu
Astronomy and Astrophysics
Astrophysics
184
Binary Stars, Double Stars, Star Distribution, Stellar Mass, Galactic Structure, Star Formation Rate, Stellar Evolution, Stellar Luminosity, Stellar Models
Scientific paper
Among the 4908 stellar systems which have at least one resolvable component brighter than V = 6.00 are 115 systems with two or more resolvable components both brighter than V = 6.00. These bright stellar systems, both single and double, are modeled by a distribution convolving (1) formulas from theoretical models for stellar evolution, including giants as well as main-sequence stars, (2) an initial mass function and birth rate function, (3) a density distribution of stars as a function of distance from the Galactic plane, and (4) a distribution of mass ratios and orbital separations. One reasonably firm conclusion is that masses, even in wide binaries, are correlated: there are too many doubly bright visual binaries (DBVBs), by a factor of 3-5, to agree with the hypothesis that the component masses are selected independently from the same IMF or luminosity function. Another conclusion is that the number of DBVBs per decibel of separation a (absolute, not apparent) is not constant in the range a = 10-100,000 AU, but instead decreases slowly with increasing a.
Eggleton Peter P.
Fitchett Michael J.
Tout Christopher A.
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