Michela Mapelli
Published 2021-05-26Version 1
We review the main physical processes that lead to the formation of stellar binary black holes (BBHs) and to their merger. BBHs can form from the isolated evolution of massive binary stars. The physics of core-collapse supernovae and the process of common envelope are two of the main sources of uncertainty about this formation channel. Alternatively, two black holes can form a binary by dynamical encounters in a dense star cluster. The dynamical formation channel leaves several imprints on the mass, spin and orbital properties of BBHs.
Comments: Mini review. Invited contribution to the volume "Gravitational Waves: A New Window to the Universe", published in Frontiers in Astronomy and Space Science. Guest Editors: Rosalba Perna and Bruno Giacomazzo. Journal-ref: Frontiers in Astronomy and Space Sciences, Volume 7, id.38 (2020)
Black Holes: The Next Generation
The spin and mass ratio affects the gravitational waveforms of binary black hole mergers with a total system mass of 12-130 $\rm{M}_\odot$
On the effective spin-mass ratio '$χ_{\rm eff}-q$' relation of binary black hole mergers that evolved in isolation
![QR code for arXiv:2105.12455 [astro-ph.HE]](http://oss.arxitics.com/images/favicon.svg)