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Numerical Evolution of Single, Binary and Triple Stars

Published online by Cambridge University Press:  01 September 2007

Peter P. Eggleton
Peter P. Eggleton*
Affiliation:
Institute of Geophysics and Planetary Physics Physics and Allied Technologies Division Lawrence Livermore National Laboratory, 7000 East Ave, Livermore, CA94551, USA email: ppe@igpp.ucllnl.org
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Abstract

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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.

Keywords

stars: evolutionstars: binaries: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S246: Dynamical Evolution of Dense Stellar Systems , September 2007 , pp. 228 - 232
Copyright
Copyright © International Astronomical Union 2008

References

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