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This study presents detailed evolutionary models of massive binary star systems that can produce merging black holes through stable mass transfer between the stars. By tracking the complete evolution from initial formation through black hole creation, including how mass and rotation are exchanged between the stars, the researchers show that this "stable mass transfer channel" naturally produces black holes with masses and spins matching those detected by gravitational wave observatories in the 10-25 solar mass range. The models include previously omitted physics such as internal stellar rotation and detailed chemical evolution of the mass-receiving star, which proves critical for determining the final black hole properties.
Why it matters
These findings help explain the origin of gravitational wave signals detected by LIGO and similar observatories, addressing a fundamental question about how binary black holes form in nature. Since many progenitor systems of this type exist in the universe, this formation channel likely contributes significantly to the observed population of merging black holes.
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⚠️ Preprint – Noch nicht peer-reviewed
Dieser Artikel wurde noch nicht von unabhängigen Experten begutachtet. Die Ergebnisse sind vorläufig und sollten mit Vorsicht interpretiert werden.
Abstract: The vast majority of massive binary systems in the universe is evidently unsuited to produce merging binary black holes. However, several narrow evolutionary paths of isolated massive binaries towards this goal have recently been identified. Due to the high degree of simplification and assumptions applied in previous modelling of these paths, conclusions remained vague so far. For one of these paths, the stable mass transfer channel, we now construct detailed binary evolution models which include internal differential rotation as well as mass and angular momentum transfer between the stars, all the way from the zero-age main sequence to the formation of the black holes, only skipping the rapid late burning stages. This allows us to follow the mass and chemical structure evolution of the mass accreting component, which turns out to have a key influence on the phase of reverse mass transfer, that allows the obtained black hole spins and mass ratios to naturally fall into the regime observed for the gravitational-wave source in the 10–25$M_odot$ primary black hole mass range. As for this channel, also a large number of progenitor binaries are known, we conclude that it likely contributes to the observed population of gravitational wave sources.
Source: Stable mass transfer in massive binaries leading to merging black holes