Bimodal black-hole mass distribution and chirp masses of binary black-hole mergers

TL;DR

This paper demonstrates that binary-stripped stars produce a bimodal black-hole mass spectrum with characteristic masses around 9 and 16 solar masses, which explains observed features in gravitational-wave data.

Contribution

It reveals a link between binary stellar evolution, core burning processes, and the resulting black-hole mass distribution, matching current gravitational-wave observations.

Findings

Bimodal black-hole mass spectrum with peaks at ~9 and 16 solar masses.

Corresponding features in the chirp-mass distribution of binary black-hole mergers.

Agreement between model predictions and gravitational-wave observations.

Abstract

In binary black-hole mergers from isolated binary-star evolution, both black holes are from progenitor stars that have lost their hydrogen-rich envelopes by binary mass transfer. Envelope stripping is known to affect the pre-supernova core structures of such binary-stripped stars and thereby their final fates and compact remnant masses. In this paper, we show that binary-stripped stars give rise to a bimodal black-hole mass spectrum with characteristic black-hole masses of about $9\,\mathrm{M}_\odot$ and $16\,\mathrm{M}_\odot$ across a large range of metallicities. The bimodality is linked to carbon and neon burning becoming neutrino-dominated, which results in interior structures that are difficult to explode and likely lead to black hole formation. The characteristic black-hole masses from binary-stripped stars have corresponding features in the chirp-mass distribution of binary black-hole mergers: peaks at about $8$ and $14\,\mathrm{M}_\odot$, and a dearth in between these masses. Current gravitational-wave observations of binary black-hole mergers show evidence for a gap at $10\text{--}12\,\mathrm{M}_\odot$ and peaks at $8$ and $14\,\mathrm{M}_\odot$ in the chirp-mass distribution. These features are in agreement with our models of binary-stripped stars. In the future, they may be used to constrain the physics of late stellar evolution and supernova explosions, and may even help measure the cosmological expansion of the Universe.