Common envelope evolution of massive stars

Paul M. Ricker; Frank X. Timmes; Ronald E. Taam; Ronald F. Webbink

doi:10.1017/S1743921318007433

Common envelope evolution of massive stars

Paul M. Ricker, Frank X. Timmes, Ronald E. Taam, Ronald F. Webbink

Physics and Astronomy

Research output: Contribution to journal › Article › peer-review

Abstract

The discovery via gravitational waves of binary black hole systems with total masses greater than 60M_Ehas 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 "30-40_E and a black hole with mass "30-40_E. 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.

Original language	English (US)
Pages (from-to)	449-454
Number of pages	6
Journal	Proceedings of the International Astronomical Union
DOIs	https://doi.org/10.1017/S1743921318007433
State	Accepted/In press - 2019

Keywords

hydrodynamics
stars: Binaries: Close
stars: Evolution

ASJC Scopus subject areas

Medicine (miscellaneous)
Astronomy and Astrophysics
Nutrition and Dietetics
Public Health, Environmental and Occupational Health
Space and Planetary Science

UN SDGs

This output contributes to the following UN Sustainable Development Goals (SDGs)

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10.1017/S1743921318007433

Cite this

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title = "Common envelope evolution of massive stars",

abstract = "The discovery via gravitational waves of binary black hole systems with total masses greater than 60MEhas 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 {"}30-40E and a black hole with mass {"}30-40E. 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 = "hydrodynamics, stars: Binaries: Close, stars: Evolution",

author = "Ricker, {Paul M.} and Timmes, {Frank X.} and Taam, {Ronald E.} and Webbink, {Ronald F.}",

year = "2019",

doi = "10.1017/S1743921318007433",

language = "English (US)",

pages = "449--454",

journal = "Proceedings of the International Astronomical Union",

issn = "1743-9213",

publisher = "Cambridge University Press",

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TY - JOUR

T1 - Common envelope evolution of massive stars

AU - Ricker, Paul M.

AU - Timmes, Frank X.

AU - Taam, Ronald E.

AU - Webbink, Ronald F.

PY - 2019

Y1 - 2019

N2 - The discovery via gravitational waves of binary black hole systems with total masses greater than 60MEhas 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 "30-40E and a black hole with mass "30-40E. 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.

AB - The discovery via gravitational waves of binary black hole systems with total masses greater than 60MEhas 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 "30-40E and a black hole with mass "30-40E. 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.

KW - hydrodynamics

KW - stars: Binaries: Close

KW - stars: Evolution

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DO - 10.1017/S1743921318007433

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EP - 454

JO - Proceedings of the International Astronomical Union

JF - Proceedings of the International Astronomical Union

SN - 1743-9213

ER -

Common envelope evolution of massive stars

Abstract

Keywords

ASJC Scopus subject areas

UN SDGs

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