Presupernova Evolution and Explosive Nucleosynthesis of Rotating Massive Stars in the Metallicity Range −3 ≤ [Fe/H] ≤ 0
By M. Limongi, A. Chieffi. Astrophysical Journal Supplement Series, 2018
323 citations recorded by the source corpus.
We present a new grid of presupernova models of massive stars extending in mass between 13 and 120 , covering four metallicities (i.e., [Fe/H] = 0, −1, −2, and −3) and three initial rotation velocities (i.e., 0, 150, and 300 km s−1). The explosion has been simulated following three different assumptions in order to show how the yields depend on the remnant mass−initial mass relation. An extended network from H to Bi is fully coupled to the physical evolution of the models. The main results can be summarized as follows. (a) At solar metallicity, the maximum mass exploding as a red supergiant (RSG) is of the order of 17 in the nonrotating case, with the more massive stars exploding as Wolf–Rayet (WR) stars. All rotating models, conversely, explode as WR stars. (b) The interplay between the core He-burning and the H-burning shell, triggered by the rotation-induced instabilities, drives the synthesis of a large primary amount of all the products of CNO, not just . A fraction of them greatly enriches the radiative part of the He core (and is responsible for the large production of F), and a fraction enters the convective core, leading therefore to an important primary neutron flux able to synthesize heavy nuclei up to Pb. (c) In our scenario, remnant masses of the order of those inferred from the first detections of gravitational waves (GW 150914, GW 151226, GW 170104, GW 170814) are predicted at all metallicities for none or moderate initial rotation velocities.
Subfields: Astronomy and Astrophysics, Molecular Biology
View Paper: https://www.semanticscholar.org/paper/b9cd0a66d49324432f04d97e3086cdabb1be3926
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In Astronomy and Astrophysics
- Michela Mapelli
- N. Giacobbo
- Mario Spera
- D. Holz
- Ilya Mandel
- Krzysztof Belczyński
- Maya Fishbach
- Chris L. Fryer
In Molecular Biology
Citations in the corpus
- Origin of the heaviest elements: The rapid neutron-capture process (2019, background): “4 (see e.g. Woosley et al., 2002; Woosley and Heger, 2007; Limongi and Chieffi, 2018) before type Ia supernovae set”
- GWTC-2.1: Deep extended catalog of compact binary coalescences observed by LIGO and Virgo during the first half of the third observing run (2021, background): “[273] Marco Limongi and Alessandro Chieffi, “Presupernova Evolution and Explosive Nucleosynthesis of Rotating Massive Stars in the Metallicity Range -3 ≤ [Fe/H] ≤ 0,” Astrophys.”
- Evolutionary roads leading to low effective spins, high black hole masses, and O1/O2 rates for LIGO/Virgo binary black holes (2017, background): “…lower-mass limit corresponds to the pair-instability pulsation supernova effects on the presupernova star and on the remnant BH mass (Woosley 2017; Limongi & Chieffi 2018; Belczynski et al. 2020), while the upper mass limit corresponds to the end of the pair-instability supernova process, that is…”
- Merging black hole binaries with the SEVN code (2018, background): “Stellar rotation (e.g. Limongi 2017; Limongi & Chieffi 2018), magnetic fields (Petit et al. 2017), pair-instability SNe (PISNe), and pulsational pair-instability SNe (PPISNe) (Belczynski et al. 2016b; Spera & Mapelli 2017; Woosley 2017) also affect this picture.”