2024/08/21 by Masaru Shibata, Shibata, Masaru, Sho Fujibayashi +5 · 2 citations
Physics and Astronomy · #Astrophysical Phenomena and Observations #Cosmology and Gravitation Theories #FOS: Physical sciences #General Relativity and Quantum Cosmology (gr-qc) #High Energy Astrophysical Phenomena (astro-ph.HE) #Pulsars and Gravitational Waves Research
paper · doi:10.48550/arxiv.2408.11577
openalex publication_date 2024/08/21 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
The dependence of the final fate of supermassive star (SMS) cores on their mass and angular momentum is studied with simple modeling. SMS cores in the hydrogen burning phase encounter the general relativistic instability during the stellar evolution if the mass is larger than ∼ 3 × 104M_\odot. Spherical SMS cores in the helium burning phase encounter the general relativistic instability prior to the onset of the electron-positron pair instability if the mass is larger than ∼ 1× 104M_\odot. For rapidly rotating SMS cores, these values for the threshold mass are enhanced by up to a factor of ∼ 5, and thus, for SMSs with mass smaller than ∼ 104M_\odot the collapse is triggered by the pair-instability, irrespective of the rotation. After the onset of the general relativistic instability, SMS cores in the hydrogen burning phase with reasonable metallicity are likely to collapse to a black hole irrespective of the degree of rotation, whereas the SMS cores in the helium burning phase could explode via nuclear burning with no black hole formation, as previous works demonstrate.