Numerical Evolution of Single, Binary and Triple Stars

Details Numerical Evolution of Single, Binary and Triple Stars Numerical Evolution of Single, Binary and Triple Stars

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008iaus..246..228e&link_type=abstract

Dynamical Evolution of Dense Stellar Systems, Proceedings of the International Astronomical Union, IAU Symposium, Volume 246, p.

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Stars: Evolution, Stars: Binaries: General

Scientific paper

I discuss my stellar evolution code Ev in the context of simulations of large clusters of stars. It has long been able to handle single stars, and also binary stars up to a point. That point is far beyond what other codes are able to do, but well short of what is necessary for believable simulations. A recent version, Ev(Twin), can in principle deal with the contact phase of binary evolution, but it is not yet clear what the physical interaction is that needs to be simulated.
An upgrade, which I hope will be only a few lines, should allow it to follow Kozai cycles with tidal friction, a process that strongly influences the orbital period of close pairs that reside within wide, non-coplanar triples. However, there are many substantial gaps in the physics of even single stars, let alone binaries or triples.

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