Communication Dans Un Congrès Année : 2024

Massive binary black hole mergers from Population II and III stars

Résumé

Population III (Pop III) stars are almost metal-free stars, born from the primordial gas in the Universe. They have eluded any attempt of observation so far. Therefore, we must rely on predictions from the most advanced and detailed stellar evolutionary models to study them. The almost total absence of metals impacts their initial mass function distribution (predicted to be top-heavy), their evolutionary path, and their final fate. Moreover, they lose a negligible fraction of their mass via stellar winds during their life. Such properties make them ideal single and binary massive black hole progenitors. In this talk, I will present the new models of Pop III stars computed with the PARSEC stellar evolutionary code. Then, I will show the large sets of Pop III and Population II binary populations computed with the SEVN code used to study the main formation channel of binary black hole mergers. From the comparison, we find only mild differences between binary BH (BBH) merger properties born from Pop III and II stars, especially if we adopt the same initial mass function and orbital properties. Most BBH mergers born from Pop III and II stars have the primary BH mass below the pair-instability gap, and the maximum secondary BH mass is < 50 solar masses. Only up to about 3% (0.1%) of BBH mergers from Pop III (II) progenitors have the primary mass above the gap. Moreover, we find that, unlike metal-rich binary stars, the main formation channel of BBH mergers from Pop III and II stars involves only stable mass transfer episodes in our fiducial model. Studies like this are fundamental in advancing our understanding of binary black hole merger formation scenarios and enhancing our interpretation capabilities of data from gravitational wave detection from current and next-gen observing facilities.

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Dates et versions

insu-04838858 , version 1 (15-12-2024)

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Guglielmo Costa. Massive binary black hole mergers from Population II and III stars. EAS2024/, 0000, à renseigner, Unknown Region. ⟨insu-04838858⟩
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