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Mass loss from binary stars approaching merger

Published online by Cambridge University Press:  30 November 2022

Ondřej Pejcha Open the ORCID record for Ondřej Pejcha [Opens in a new window]
Ondřej Pejcha*
Affiliation:
Institute of Theoretical Physics, Faculty of Mathematics and Physics, Charles University, V Holešovičkách 2, 180 00 Praha 8, Czech Republic email: [email protected]
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Abstract

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Some binary stars experience common envelope evolution, which is accompanied by drastic loss of angular momentum, mass, and orbital energy and which leaves behind close binaries often involving at least one white dwarf, neutron star, or black hole. The best studied phase of common envelope is the dynamical inspiral lasting few original orbital periods. We show theoretical interpretation of observations of V1309 Sco and AT2018bwo revealing that binaries undergo substantial prolonged mass loss before the dynamical event amounting up to few solar masses. This mass loss is concentrated in the orbital plane in the form of an outflow or a circumbinary disk. Collision between this slower mass loss and the subsequent faster dynamical ejection powers a bright red transient. The resulting radiative shock helps to shape the explosion remnant and provides a site of dust and molecule formation.

Keywords

binaries: generalstars: mass lossstars: windsoutflows
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 16 , Symposium S366: The Origin of Outflows in Evolved Stars , November 2020 , pp. 159 - 164
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Copyright
© The Author(s), 2022. Published by Cambridge University Press on behalf of International Astronomical Union

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