Self-Consistent Numerical Simulations of Close Binaries

Details Self-Consistent Numerical Simulations of Close Binaries Self-Consistent Numerical Simulations of Close Binaries

Dec 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aas...19712911m&link_type=abstract

American Astronomical Society, 197th AAS Meeting, #129.11; Bulletin of the American Astronomical Society, Vol. 33, p.713

Statistics

Computation

Scientific paper

We present results from numerical simulations of close binary star systems. The computations are self-consistent in that the gravitational potential is calculated explicitly from the current density distribution throughout the hydrodynamical simulation. We assume that the evolution is adiabatic. The simulations proceed from initial conditions describing extended, polytropic fluid stars that are undergoing synchronous rotation upon circular orbits. For a subset of the simulations performed, one binary component fills its Roche lobe and the binaries have a mass ratio and / or polytropic index such that the systems are unstable to growth in any initial mass transfer rate.

Affiliated with

Also associated with

No associations

Rating

Self-Consistent Numerical Simulations of Close Binaries does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Self-Consistent Numerical Simulations of Close Binaries, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Self-Consistent Numerical Simulations of Close Binaries will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1729195