We present new evolutionary models of primordial very massive stars with initial masses ranging from 100 to 1000 M (circle dot) that extend from the main sequence to the onset of dynamical instability caused by the creation of electron-positron pairs during core C, Ne, or O burning, depending on the star's mass and metallicity. Mass loss accounts for radiation-driven winds, as well as pulsation-driven mass loss on the main sequence and during the red supergiant phase. After examining the evolutionary properties, we focus on the final outcome of the models and associated compact remnants. Stars that avoid the pair instability supernova channel should produce black holes with masses ranging from approximate to 40 to approximate to 1000 M (circle dot). In particular, stars with initial masses of about 100 M (circle dot) could leave black holes of similar or equal to 85-90 M (circle dot), values consistent with the estimated primary black hole mass of the GW190521 merger event. Overall, these results may contribute to explaining future data from next-generation gravitational-wave detectors, such as the Einstein Telescope and Cosmic Explorer, which will have access to an as-yet-unexplored black hole mass range of approximate to 10(2)-10(4) M (circle dot) in the early universe.

A Study of Primordial Very Massive Star Evolution / Volpato, Guglielmo; Marigo, Paola; Costa, Guglielmo; Bressan, Alessandro; Trabucchi, Michele; Girardi, Léo. - In: THE ASTROPHYSICAL JOURNAL. - ISSN 0004-637X. - 944:1(2023), pp. 1-14. [10.3847/1538-4357/acac91]

A Study of Primordial Very Massive Star Evolution

Costa, Guglielmo;Bressan, Alessandro;
2023-01-01

Abstract

We present new evolutionary models of primordial very massive stars with initial masses ranging from 100 to 1000 M (circle dot) that extend from the main sequence to the onset of dynamical instability caused by the creation of electron-positron pairs during core C, Ne, or O burning, depending on the star's mass and metallicity. Mass loss accounts for radiation-driven winds, as well as pulsation-driven mass loss on the main sequence and during the red supergiant phase. After examining the evolutionary properties, we focus on the final outcome of the models and associated compact remnants. Stars that avoid the pair instability supernova channel should produce black holes with masses ranging from approximate to 40 to approximate to 1000 M (circle dot). In particular, stars with initial masses of about 100 M (circle dot) could leave black holes of similar or equal to 85-90 M (circle dot), values consistent with the estimated primary black hole mass of the GW190521 merger event. Overall, these results may contribute to explaining future data from next-generation gravitational-wave detectors, such as the Einstein Telescope and Cosmic Explorer, which will have access to an as-yet-unexplored black hole mass range of approximate to 10(2)-10(4) M (circle dot) in the early universe.
2023
944
1
1
14
40
https://doi.org/10.3847/1538-4357/acac91
https://arxiv.org/abs/2212.09629
Volpato, Guglielmo; Marigo, Paola; Costa, Guglielmo; Bressan, Alessandro; Trabucchi, Michele; Girardi, Léo
File in questo prodotto:
File Dimensione Formato  
Volpato_2023_ApJ_944_40.pdf

accesso aperto

Tipologia: Versione Editoriale (PDF)
Licenza: Creative commons
Dimensione 2.38 MB
Formato Adobe PDF
2.38 MB Adobe PDF Visualizza/Apri

I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.

Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/20.500.11767/137772
Citazioni
  • ???jsp.display-item.citation.pmc??? ND
  • Scopus 9
  • ???jsp.display-item.citation.isi??? 8
social impact