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  Stripped-envelope stars in different metallicity environments - II. Type I supernovae and compact remnants

Aguilera-Dena, D. R., Müller, B., Antoniadis, J., Langer, N., Dessart, L., Vigna-Gomez, A., et al. (2023). Stripped-envelope stars in different metallicity environments - II. Type I supernovae and compact remnants. Astronomy and Astrophysics, 671: A134. doi:10.1051/0004-6361/202243519.

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Aguilera-Dena, David R., Author
Müller, Bernhard, Author
Antoniadis, John, Author
Langer, Norbert, Author
Dessart, Luc, Author
Vigna-Gomez, Alejandro1, Author           
Yoon, Sung-Chul, Author
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1Stellar Astrophysics, MPI for Astrophysics, Max Planck Society, ou_159882              

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 Abstract: Stripped-envelope stars can be observed as Wolf-Rayet (WR) stars or as less luminous hydrogen-poor stars with low mass-loss rates and transparent winds. Both types are potential progenitors of Type I core-collapse supernovae (SNe). We used grids of core-collapse models obtained from single helium stars at different metallicities to study the effects of metallicity on the transients and remnants these stars produce. We characterised the surface and core properties of our core-collapse models and investigated their ‘explodability’ using three criteria. In the cases where explosions are predicted, we estimated the ejecta mass, explosion energy, nickel mass, and neutron star (NS) mass. Otherwise, we predicted the mass of the resulting black hole (BH). We constructed a simplified population model and find that the properties of SNe and compact objects depend strongly on metallicity. The ejecta masses and explosion energies for Type Ic SNe are best reproduced by models with Z = 0.04 that exhibit strong winds during core helium burning. This implies that either their mass-loss rates are underestimated or that Type Ic SN progenitors experience mass loss through other mechanisms before exploding. The distributions of ejecta masses, explosion energies, and nickel mass for Type Ib SNe are not well reproduced by progenitor models with WR mass loss, but are better reproduced if we assume no mass loss in progenitors with luminosities below the minimum WR star luminosity. We find that Type Ic SNe become more common as metallicity increases, and that the vast majority of progenitors of Type Ib SNe must be transparent-wind stripped-envelope stars. We find that several models with pre-collapse CO masses of up to ∼30 M may form ∼3 M BHs in fallback SNe. This may have important consequences for our understanding of SNe, binary BH and NS systems, X-ray binary systems, and gravitational wave transients.

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Language(s): eng - English
 Dates: 2023-03-15
 Publication Status: Published online
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 Identifiers: DOI: 10.1051/0004-6361/202243519
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Title: Astronomy and Astrophysics
  Other : Astron. Astrophys.
Source Genre: Journal
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Publ. Info: France : EDP Sciences S A
Pages: - Volume / Issue: 671 Sequence Number: A134 Start / End Page: - Identifier: ISSN: 1432-0746
CoNE: https://pure.mpg.de/cone/journals/resource/954922828219_1