Threshold Mass of the General-relativistic Instability for Supermassive Star Cores
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 stellar evolution if the mass is larger than ∼3 × 10 ^4 M _⊙ . Spherical...
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IOP Publishing
2024-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ad93a4 |
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| author | Masaru Shibata Sho Fujibayashi Cédric Jockel Kyohei Kawaguchi |
| author_facet | Masaru Shibata Sho Fujibayashi Cédric Jockel Kyohei Kawaguchi |
| author_sort | Masaru Shibata |
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| description | 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 stellar evolution if the mass is larger than ∼3 × 10 ^4 M _⊙ . 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 × 10 ^4 M _⊙ . 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 ∼10 ^4 M _⊙ , 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 SMS cores in the helium-burning phase could explode via nuclear burning with no black hole formation, as previous works demonstrate. |
| format | Article |
| id | doaj-art-03c6915c4f184178a32f07f95e52a374 |
| institution | DOAJ |
| issn | 1538-4357 |
| language | English |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
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| series | The Astrophysical Journal |
| spelling | doaj-art-03c6915c4f184178a32f07f95e52a3742025-08-20T02:40:00ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-0197815810.3847/1538-4357/ad93a4Threshold Mass of the General-relativistic Instability for Supermassive Star CoresMasaru Shibata0https://orcid.org/0000-0002-4979-5671Sho Fujibayashi1https://orcid.org/0000-0001-6467-4969Cédric Jockel2https://orcid.org/0009-0007-7617-7178Kyohei Kawaguchi3https://orcid.org/0000-0003-4443-6984Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut) , Am Mühlenberg 1, D-14476 Potsdam-Golm, Germany; Center for Gravitational Physics and Quantum Information, Yukawa Institute for Theoretical Physics, Kyoto University , Kyoto, 606-8502, JapanMax-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut) , Am Mühlenberg 1, D-14476 Potsdam-Golm, Germany; Frontier Research Institute for Interdisciplinary Sciences, Tohoku University , Sendai 980-8578, Japan; Astronomical Institute, Graduate School of Science, Tohoku University , Sendai 980-8578, JapanMax-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut) , Am Mühlenberg 1, D-14476 Potsdam-Golm, GermanyMax-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut) , Am Mühlenberg 1, D-14476 Potsdam-Golm, Germany; Center for Gravitational Physics and Quantum Information, Yukawa Institute for Theoretical Physics, Kyoto University , Kyoto, 606-8502, Japan; Institute for Cosmic Ray Research, The University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582, JapanThe 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 stellar evolution if the mass is larger than ∼3 × 10 ^4 M _⊙ . 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 × 10 ^4 M _⊙ . 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 ∼10 ^4 M _⊙ , 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 SMS cores in the helium-burning phase could explode via nuclear burning with no black hole formation, as previous works demonstrate.https://doi.org/10.3847/1538-4357/ad93a4Massive starsSupermassive black holesGravitational collapse |
| spellingShingle | Masaru Shibata Sho Fujibayashi Cédric Jockel Kyohei Kawaguchi Threshold Mass of the General-relativistic Instability for Supermassive Star Cores The Astrophysical Journal Massive stars Supermassive black holes Gravitational collapse |
| title | Threshold Mass of the General-relativistic Instability for Supermassive Star Cores |
| title_full | Threshold Mass of the General-relativistic Instability for Supermassive Star Cores |
| title_fullStr | Threshold Mass of the General-relativistic Instability for Supermassive Star Cores |
| title_full_unstemmed | Threshold Mass of the General-relativistic Instability for Supermassive Star Cores |
| title_short | Threshold Mass of the General-relativistic Instability for Supermassive Star Cores |
| title_sort | threshold mass of the general relativistic instability for supermassive star cores |
| topic | Massive stars Supermassive black holes Gravitational collapse |
| url | https://doi.org/10.3847/1538-4357/ad93a4 |
| work_keys_str_mv | AT masarushibata thresholdmassofthegeneralrelativisticinstabilityforsupermassivestarcores AT shofujibayashi thresholdmassofthegeneralrelativisticinstabilityforsupermassivestarcores AT cedricjockel thresholdmassofthegeneralrelativisticinstabilityforsupermassivestarcores AT kyoheikawaguchi thresholdmassofthegeneralrelativisticinstabilityforsupermassivestarcores |