Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
We present the evolution and the explosion of two massive stars, 15 and 25 M _⊙ , spanning a wide range of initial rotation velocities (from 0 to 800 km s ^−1 ) and three initial metallicities: Z = 0 ([Fe/H] = −∞), 3.236 × 10 ^−7 ([Fe/H] = −5), and 3.236 × 10 ^−6 ([Fe/H] = −4). A very large nuclear...
| Main Authors: | , , |
|---|---|
| Format: | Article |
| Language: | English |
| Published: |
IOP Publishing
2024-01-01
|
| Series: | The Astrophysical Journal Supplement Series |
| Subjects: | |
| Online Access: | https://doi.org/10.3847/1538-4365/ad1686 |
| _version_ | 1827180967935082496 |
|---|---|
| author | Lorenzo Roberti Marco Limongi Alessandro Chieffi |
| author_facet | Lorenzo Roberti Marco Limongi Alessandro Chieffi |
| author_sort | Lorenzo Roberti |
| collection | DOAJ |
| description | We present the evolution and the explosion of two massive stars, 15 and 25 M _⊙ , spanning a wide range of initial rotation velocities (from 0 to 800 km s ^−1 ) and three initial metallicities: Z = 0 ([Fe/H] = −∞), 3.236 × 10 ^−7 ([Fe/H] = −5), and 3.236 × 10 ^−6 ([Fe/H] = −4). A very large nuclear network of 524 nuclear species extending up to Bi has been adopted. Our main findings may be summarized as follows: (a) rotating models above Z = 0 are able to produce nuclei up to the neutron closure shell N = 50, and in a few cases up to N = 82; (b) rotation drastically inhibits the penetration of the He convective shell in the H-rich mantle, a phenomenon often found in zero metallicity nonrotating massive stars; (c) vice versa, rotation favors the penetration of the O convective shell in the C-rich layers with the consequence of significantly altering the yields of the products of the C, Ne, and O burning; (d) none of the models that reach the critical velocity while in H burning lose more the 1 M _⊙ in this phase; (e) conversely, almost all models able to reach their Hayashi track exceed the Eddington luminosity and dynamically lose almost all their H-rich mantle. These models suggest that rotating massive stars may have contributed significantly to the synthesis of the heavy nuclei in the first phase of enrichment of the interstellar medium, i.e., at early times. |
| first_indexed | 2024-03-08T07:39:54Z |
| format | Article |
| id | doaj.art-349243b4d91944838551a78aea81d4de |
| institution | Directory Open Access Journal |
| issn | 0067-0049 |
| language | English |
| last_indexed | 2025-03-21T05:39:20Z |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal Supplement Series |
| spelling | doaj.art-349243b4d91944838551a78aea81d4de2024-07-24T11:54:49ZengIOP PublishingThe Astrophysical Journal Supplement Series0067-00492024-01-0127022810.3847/1538-4365/ad1686Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest NucleiLorenzo Roberti0https://orcid.org/0000-0003-0390-8770Marco Limongi1https://orcid.org/0000-0003-0636-7834Alessandro Chieffi2https://orcid.org/0000-0002-3589-3203Konkoly Observatory, Research Centre for Astronomy and Earth Sciences , HUN-REN, Konkoly Thege Miklós út 15-17, H-1121 Budapest, Hungary; CSFK, MTA Centre of Excellence , Budapest, Konkoly Thege Miklós út 15-17, H-1121, Hungary; Istituto Nazionale di Astrofisica—Osservatorio Astronomico di Roma , Via Frascati 33, I-00040, Monteporzio Catone, ItalyIstituto Nazionale di Astrofisica—Osservatorio Astronomico di Roma , Via Frascati 33, I-00040, Monteporzio Catone, Italy; Kavli Institute for the Physics and Mathematics of the Universe , Todai Institutes for Advanced Study, University of Tokyo, Kashiwa, 277-8583 (Kavli IPMU, WPI), Japan; INFN. Sezione di Perugia , via A. Pascoli s/n, I-06125 Perugia, ItalyINFN. Sezione di Perugia , via A. Pascoli s/n, I-06125 Perugia, Italy; Istituto Nazionale di Astrofisica—Istituto di Astrofisica e Planetologia Spaziali , Via Fosso del Cavaliere 100, I-00133, Roma, Italy; Monash Centre for Astrophysics (MoCA), School of Mathematical Sciences, Monash University , Victoria 3800, AustraliaWe present the evolution and the explosion of two massive stars, 15 and 25 M _⊙ , spanning a wide range of initial rotation velocities (from 0 to 800 km s ^−1 ) and three initial metallicities: Z = 0 ([Fe/H] = −∞), 3.236 × 10 ^−7 ([Fe/H] = −5), and 3.236 × 10 ^−6 ([Fe/H] = −4). A very large nuclear network of 524 nuclear species extending up to Bi has been adopted. Our main findings may be summarized as follows: (a) rotating models above Z = 0 are able to produce nuclei up to the neutron closure shell N = 50, and in a few cases up to N = 82; (b) rotation drastically inhibits the penetration of the He convective shell in the H-rich mantle, a phenomenon often found in zero metallicity nonrotating massive stars; (c) vice versa, rotation favors the penetration of the O convective shell in the C-rich layers with the consequence of significantly altering the yields of the products of the C, Ne, and O burning; (d) none of the models that reach the critical velocity while in H burning lose more the 1 M _⊙ in this phase; (e) conversely, almost all models able to reach their Hayashi track exceed the Eddington luminosity and dynamically lose almost all their H-rich mantle. These models suggest that rotating massive stars may have contributed significantly to the synthesis of the heavy nuclei in the first phase of enrichment of the interstellar medium, i.e., at early times.https://doi.org/10.3847/1538-4365/ad1686S-processStellar evolutionStellar rotationMassive starsCore-collapse supernovaeNucleosynthesis |
| spellingShingle | Lorenzo Roberti Marco Limongi Alessandro Chieffi Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei The Astrophysical Journal Supplement Series S-process Stellar evolution Stellar rotation Massive stars Core-collapse supernovae Nucleosynthesis |
| title | Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei |
| title_full | Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei |
| title_fullStr | Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei |
| title_full_unstemmed | Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei |
| title_short | Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei |
| title_sort | zero and extremely low metallicity rotating massive stars evolution explosion and nucleosynthesis up to the heaviest nuclei |
| topic | S-process Stellar evolution Stellar rotation Massive stars Core-collapse supernovae Nucleosynthesis |
| url | https://doi.org/10.3847/1538-4365/ad1686 |
| work_keys_str_mv | AT lorenzoroberti zeroandextremelylowmetallicityrotatingmassivestarsevolutionexplosionandnucleosynthesisuptotheheaviestnuclei AT marcolimongi zeroandextremelylowmetallicityrotatingmassivestarsevolutionexplosionandnucleosynthesisuptotheheaviestnuclei AT alessandrochieffi zeroandextremelylowmetallicityrotatingmassivestarsevolutionexplosionandnucleosynthesisuptotheheaviestnuclei |