http://arxiv.org/abs/1811.03656
The discovery via gravitational waves of binary black hole systems with total masses greater than $60M_\odot$ has raised interesting questions for stellar evolution theory. Among the most promising formation channels for these systems is one involving a common envelope binary containing a low metallicity, core helium burning star with mass $\sim 80-90M_\odot$ and a black hole with mass $\sim 30-40M_\odot$. For this channel to be viable, the common envelope binary must eject more than half the giant star’s mass and reduce its orbital separation by as much as a factor of 80. We discuss issues faced in numerically simulating the common envelope evolution of such systems and present a 3D AMR simulation of the dynamical inspiral of a low-metallicity red supergiant with a massive black hole companion.
P. Ricker, F. Timmes, R. Taam, et. al.
Mon, 12 Nov 18
48/68
Comments: 6 pages, 3 figures, oral contribution: IAU Symposium 346 “High Mass X-ray Binaries: illuminating the passage from massive binaries to merging compact objects”, Vienna, Austria, 27-31 August 2018
You must be logged in to post a comment.