Theoretical Studies of Binaries in Astrophysics

This thesis introduces and summarizes four papers dealing with computer simulations of astrophysical processes involving binaries. The first part gives the rational and theoretical background to these papers.

In paper I and II a statistical approach to studying eclipsing binaries is described. By using population synthesis models for binaries the probabilities for eclipses are calculated for different luminosity classes of binaries. These are compared with Hipparcos data and they agree well if one uses a standard input distribution for the orbit sizes. If one uses a random pairing model, where both companions are independently picked from an IMF, one finds too few eclipsing binaries by an order of magnitude.

In paper III we investigate a possible scenario for the origin of the stars observed close to the centre of our galaxy, called S~stars. We propose that a cluster falls radially towards the central black hole. The binaries within the cluster can then,

if they have small impact parameters, be broken up by the black hole's tidal field and one of the components of the binary will be captured by the black hole.

Paper~IV investigates how the onset of mass transfer in eccentric binaries depends on the eccentricity. To do this we have developed a new two-phase SPH scheme where very light particles are at the outer edge of our simulated star. This enables us to get a much better resolution of the very small mass that is transferred in close binaries. Our simulations show that the minimum required distance between the stars to have mass transfer decreases with the eccentricity.