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Dynamical versus isolated formation channels of gravitational wave sources

Published online by Cambridge University Press:  30 December 2019

Michela Mapelli
Michela Mapelli*
Affiliation:
Dipartimento di Fisica e Astronomia G. Galilei, Università degli Studi di Padova, Vicolo dell’Osservatorio 3, I–35122, Padova, Italy email: michela.mapelli@unipd.it Institut für Astro-und Teilchenphysik, Universität Innsbruck, Technikerstrasse 25/8, A–6020 Innsbruck, Austria INAF – Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, I–35142 Padova, Italy INFN – Sezione di Padova, Via F. Marzolo 8, I–35131 Padova, Italy
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Abstract

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What are the formation channels of merging black holes and neutron stars? The first two observing runs of Advanced LIGO and Virgo give us invaluable insights to address this question, but a new approach to theoretical models is required, in order to match the challenges posed by the new data. In this review, I discuss the impact of stellar winds, core-collapse and pair instability supernovae on the formation of compact remnants in both isolated and dynamically formed binaries. Finally, I show that dynamical processes, such as the runaway collision scenario and the Kozai-Lidov mechanism, leave a clear imprint on the demography of merging systems.

Keywords

black hole physicsgravitational waves(stars:) binaries: generalstellar dynamicsstars: windsgalaxies: star clusters

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