EDP Sciences
Free access
Volume 446, Number 3, February II 2006
Page(s) 1071 - 1079
Section Stellar structure and evolution
DOI http://dx.doi.org/10.1051/0004-6361:20053543
A&A 446, 1071-1079 (2006)
DOI: 10.1051/0004-6361:20053543

Evolution of interacting binaries with a B type primary at birth

W. Van Rensbergen, C. De Loore and K. Jansen

Astrophysical Institute, Vrije Universiteit Brussel, Pleinlaan 2, 1050 Brussels, Belgium
    e-mail: wvanrens@vub.ac.be; cdeloore@pandora.be; kijansen@vub.ac.be

(Received 31 May 2005 / Accepted 13 September 2005)

We revisited the analytical expression for the mass ratio distribution for non-evolved binaries with a B type primary. Selection effects governing the observations were taken into account in order to compare theory with observations. Theory was optimized so as to fit best with the observed q-distribution of SB1s and SB2s. The accuracy of this theoretical mass ratio distribution function is severely hindered by the uncertainties on the observations. We present a library of evolutionary computations for binaries with a B type primary at birth. Some liberal computations including loss of mass and angular momentum during binary evolution are added to an extensive grid of conservative calculations. Our computations are compared statistically to the observed distributions of orbital periods and mass ratios of Algols. Conservative Roche Lobe Over Flow (RLOF) reproduces the observed distribution of orbital periods but fails to explain the observed mass ratios in the range q $\in$ $\lbrack$0.4-1$\rbrack$. In order to obtain a better fit the binaries have to lose a significant amount of matter, without losing much angular momentum.

Key words: stars: binaries: close -- stars: evolution -- stars: fundamental parameters -- stars: mass-loss -- stars: luminosity function, mass function -- stars: statistics

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