Black Hole Formation Accompanied by the Supernova Explosion of a 40 M ⊙ Progenitor Star
We have simulated the collapse and evolution of the core of a solar-metallicity 40 M _⊙ star and find that it explodes vigorously by the neutrino mechanism, despite its very high “compactness.” Within ∼1.5 s of explosion, a black hole forms. The explosion is very asymmetrical and has a total explosi...
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/acfc1c |
| _version_ | 1797644263728611328 |
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| author | Adam Burrows David Vartanyan Tianshu Wang |
| author_facet | Adam Burrows David Vartanyan Tianshu Wang |
| author_sort | Adam Burrows |
| collection | DOAJ |
| description | We have simulated the collapse and evolution of the core of a solar-metallicity 40 M _⊙ star and find that it explodes vigorously by the neutrino mechanism, despite its very high “compactness.” Within ∼1.5 s of explosion, a black hole forms. The explosion is very asymmetrical and has a total explosion energy of ∼1.6 × 10 ^51 erg. At black hole formation, its baryon mass is ∼2.434 M _⊙ and gravitational mass is 2.286 M _⊙ . Seven seconds after black hole formation, an additional ∼0.2 M _⊙ is accreted, leaving a black hole baryon mass of ∼2.63 M _⊙ . A disk forms around the proto−neutron star, from which a pair of neutrino-driven jets emanates. These jets accelerate some of the matter up to speeds of ∼45,000 km s ^−1 and contain matter with entropies of ∼50. The large spatial asymmetry in the explosion results in a residual black hole recoil speed of ∼1000 km s ^−1 . This novel black hole formation channel now joins the other black hole formation channel between ∼12 and ∼15 M _⊙ discovered previously and implies that the black hole/neutron star birth ratio for solar-metallicity stars could be ∼20%. However, one channel leaves black holes in perhaps the ∼5–15 M _⊙ range with low kick speeds, while the other leaves black holes in perhaps the ∼2.5–3.0 M _⊙ mass range with high kick speeds. However, even ∼8.8 s after core bounce the newly formed black hole is still accreting at a rate of ∼2 × 10 ^−2 M _⊙ s ^−1 , and whether the black hole eventually achieves a significantly larger mass over time is yet to be determined. |
| first_indexed | 2024-03-11T14:27:58Z |
| format | Article |
| id | doaj.art-2c9e82304a7b4089843da6e3e5499ce2 |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-11T14:27:58Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-2c9e82304a7b4089843da6e3e5499ce22023-10-31T12:32:41ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-0195726810.3847/1538-4357/acfc1cBlack Hole Formation Accompanied by the Supernova Explosion of a 40 M ⊙ Progenitor StarAdam Burrows0https://orcid.org/0000-0002-3099-5024David Vartanyan1https://orcid.org/0000-0003-1938-9282Tianshu Wang2https://orcid.org/0000-0002-0042-9873Department of Astrophysical Sciences, Princeton University , NJ 08544, USA ; burrows@astro.princeton.edu; School of Natural Sciences, Institute for Advanced Study , Princeton, NJ 08540, USACarnegie Observatories, 813 Santa Barbara St., Pasadena, CA 91101, USADepartment of Astrophysical Sciences, Princeton University , NJ 08544, USA ; burrows@astro.princeton.eduWe have simulated the collapse and evolution of the core of a solar-metallicity 40 M _⊙ star and find that it explodes vigorously by the neutrino mechanism, despite its very high “compactness.” Within ∼1.5 s of explosion, a black hole forms. The explosion is very asymmetrical and has a total explosion energy of ∼1.6 × 10 ^51 erg. At black hole formation, its baryon mass is ∼2.434 M _⊙ and gravitational mass is 2.286 M _⊙ . Seven seconds after black hole formation, an additional ∼0.2 M _⊙ is accreted, leaving a black hole baryon mass of ∼2.63 M _⊙ . A disk forms around the proto−neutron star, from which a pair of neutrino-driven jets emanates. These jets accelerate some of the matter up to speeds of ∼45,000 km s ^−1 and contain matter with entropies of ∼50. The large spatial asymmetry in the explosion results in a residual black hole recoil speed of ∼1000 km s ^−1 . This novel black hole formation channel now joins the other black hole formation channel between ∼12 and ∼15 M _⊙ discovered previously and implies that the black hole/neutron star birth ratio for solar-metallicity stars could be ∼20%. However, one channel leaves black holes in perhaps the ∼5–15 M _⊙ range with low kick speeds, while the other leaves black holes in perhaps the ∼2.5–3.0 M _⊙ mass range with high kick speeds. However, even ∼8.8 s after core bounce the newly formed black hole is still accreting at a rate of ∼2 × 10 ^−2 M _⊙ s ^−1 , and whether the black hole eventually achieves a significantly larger mass over time is yet to be determined.https://doi.org/10.3847/1538-4357/acfc1cCore-collapse supernovae |
| spellingShingle | Adam Burrows David Vartanyan Tianshu Wang Black Hole Formation Accompanied by the Supernova Explosion of a 40 M ⊙ Progenitor Star The Astrophysical Journal Core-collapse supernovae |
| title | Black Hole Formation Accompanied by the Supernova Explosion of a 40 M ⊙ Progenitor Star |
| title_full | Black Hole Formation Accompanied by the Supernova Explosion of a 40 M ⊙ Progenitor Star |
| title_fullStr | Black Hole Formation Accompanied by the Supernova Explosion of a 40 M ⊙ Progenitor Star |
| title_full_unstemmed | Black Hole Formation Accompanied by the Supernova Explosion of a 40 M ⊙ Progenitor Star |
| title_short | Black Hole Formation Accompanied by the Supernova Explosion of a 40 M ⊙ Progenitor Star |
| title_sort | black hole formation accompanied by the supernova explosion of a 40 m ⊙ progenitor star |
| topic | Core-collapse supernovae |
| url | https://doi.org/10.3847/1538-4357/acfc1c |
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