Astronomy and Astrophysics – Astrophysics
Scientific paper
2005-12-06
Astrophys.J.643:381-401,2006
Astronomy and Astrophysics
Astrophysics
47 pages, 11 figures, submitted to the Astrophysical Journal. See http://www.phys.lsu.edu/faculty/tohline/astroph/dmtf05 for h
Scientific paper
10.1086/500384
Hydrodynamical simulations of semi-detached, polytropic binary stars are presented in an effort to study the onset and stability of dynamical mass transfer events. Initial, synchronously rotating equilibrium models are constructed using a self-consistent-field technique and then evolved with an Eulerian hydrodynamics code in a fully self-consistent manner. We describe code improvements introduced over the past few years that permit us to follow dynamical mass-transfer events through more than 30 orbits. Mass-transfer evolutions are presented for two different initial configurations: A dynamically unstable binary with initial mass ratio (donor/accretor) $q_0 = 1.3$ that leads to a complete merger in $\sim 10$ orbits; and a double-degenerate binary with initial mass ratio $q_0 = 0.5$ that, after some initial unstable growth of mass transfer, tends to separate as the mass-transfer rate levels off.
D'Souza Mario C. R.
Frank Juhan
Motl Patrick M.
Tohline Joel E.
No associations
LandOfFree
Numerical Simulations of the Onset and Stability of Dynamical Mass Transfer in 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 Numerical Simulations of the Onset and Stability of Dynamical Mass Transfer in Binaries, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Numerical Simulations of the Onset and Stability of Dynamical Mass Transfer in Binaries will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-697446