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On the Pair-instabi...
On the Pair-instability Supernova Origin of J1010+2358
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- Skuladottir, Asa (författare)
- Univ Firenze, Dipartimento Fis & Astron, Via G Sansone 1, I-50019 Sesto Fiorentino, Italy.
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- Koutsouridou, Ioanna (författare)
- Univ Firenze, Dipartimento Fis & Astron, Via G Sansone 1, I-50019 Sesto Fiorentino, Italy.
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- Vanni, Irene (författare)
- Univ Firenze, Dipartimento Fis & Astron, Via G Sansone 1, I-50019 Sesto Fiorentino, Italy.
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- Amarsi, Anish M. (författare)
- Uppsala universitet,Teoretisk astrofysik
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- Lucchesi, Romain (författare)
- Univ Firenze, Dipartimento Fis & Astron, Via G Sansone 1, I-50019 Sesto Fiorentino, Italy.
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- Aguado, David S. (författare)
- Inst Astrofis Canarias, Via Lactea, San Cristobal la Laguna 38205, Tenerife, Spain.;Univ Laguna, Dept Astrofis, San Cristobal la Laguna 38206, Tenerife, Spain.
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- Salvadori, Stefania (författare)
- Univ Firenze, Dipartimento Fis & Astron, Via G Sansone 1, I-50019 Sesto Fiorentino, Italy.
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Univ Firenze, Dipartimento Fis & Astron, Via G Sansone 1, I-50019 Sesto Fiorentino, Italy Teoretisk astrofysik (creator_code:org_t)
- Institute of Physics Publishing (IOPP), 2024
- 2024
- Engelska.
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Ingår i: Astrophysical Journal Letters. - : Institute of Physics Publishing (IOPP). - 2041-8205 .- 2041-8213. ; 968:2
- Relaterad länk:
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https://doi.org/10.3...
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https://uu.diva-port... (primary) (Raw object)
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https://urn.kb.se/re...
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https://doi.org/10.3...
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Abstract
Ämnesord
Stäng
- The first (Population III) stars formed only out of H and He and were likely more massive than present-day stars. Massive Population III stars in the range 140-260 M-circle dot are predicted to end their lives as pair-instability supernovae (PISNe), enriching the environment with a unique abundance pattern, with high ratios of odd to even elements. Recently, the most promising candidate for a pure descendant of a zero-metallicity massive PISN (260 M-circle dot) was discovered by the LAMOST survey, the star J1010+2358. However, key elements to verify the high PISN contribution, C and Al, were missing from the analysis. To rectify this, we obtained and analyzed a high-resolution Very Large Telescope/UVES spectrum, correcting for 3D and/or non-local thermodynamic equilibrium effects. Our measurements of both C and Al give much higher values (similar to 1 dex) than expected from a 260 M-circle dot PISN. Furthermore, we find significant discrepancies with the previous analysis and therefore a much less pronounced odd-even pattern. Our results show that J1010+2358 cannot be a pure descendant of a 260 M-circle dot PISN. Instead, we find that the best-fit model consists of a 13 M-circle dot Population II core-collapse supernova combined with a Population III supernova. Alternative, less favored solutions (chi(2)/chi(2)(best) approximate to 2.3) include a 50% contribution from a 260 M-circle dot PISN or a 40% contribution from a Population III Type Ia supernova. Ultimately, J1010+2358 is certainly a unique star giving insights into the earliest chemical enrichment; however, this star is not a pure PISN descendant.
Ämnesord
- NATURVETENSKAP -- Fysik -- Astronomi, astrofysik och kosmologi (hsv//swe)
- NATURAL SCIENCES -- Physical Sciences -- Astronomy, Astrophysics and Cosmology (hsv//eng)
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