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Common envelope evolution of massive stars

Published online by Cambridge University Press:  30 December 2019

Paul M. Ricker Open the ORCID record for Paul M. Ricker [Opens in a new window] ,
Frank X. Timmes ,
Ronald E. Taam  and
Ronald F. Webbink
Paul M. Ricker
Affiliation:
Department of Astronomy, University of Illinois, 1002 W. Green St., Urbana, IL 61801 USA emails: [email protected], [email protected]
Frank X. Timmes
Affiliation:
School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287-1404 USA email: [email protected]
Ronald E. Taam
Affiliation:
Department of Physics and Astronomy, Northwestern University, 2145 Sheridan Road, Evanston, IL 60208 USA email: [email protected]
Ronald F. Webbink
Affiliation:
Department of Astronomy, University of Illinois, 1002 W. Green St., Urbana, IL 61801 USA emails: [email protected], [email protected]
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Abstract

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The discovery via gravitational waves of binary black hole systems with total masses greater than 60Mʘ 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 ⁓30 – 40Mʘ and a black hole with mass ⁓30 – 40Mʘ. 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.

Keywords

stars: binaries: closestars: evolutionhydrodynamics
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S346: High-mass X-ray Binaries: Illuminating the Passage from Massive Binaries to Merging Compact Objects , August 2018 , pp. 449 - 454
Copyright
© International Astronomical Union 2019 

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