Journal
ASTROPHYSICAL JOURNAL LETTERS
Volume 905, Issue 2, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.3847/2041-8213/abcb96
Keywords
Stellar evolution; Massive stars; Stellar mass loss; Population III stars; Black holes
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Funding
- Japan Society for the Promotion of Science [17H01130, 17K05380, 19K03907, 20H05249]
- Grants-in-Aid for Scientific Research [17K05380, 17H01130, 20H05249] Funding Source: KAKEN
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Since the discovery of GW190521, several proposals have been put forward to explain the formation of a black hole (BH) in the mass gap caused by (pulsational) pair-instability (PPI), M = 65-130 M-circle dot. We calculate the mass ejection of Population III stars by the PPI process using a stellar evolution and hydrodynamical code. If a relatively small, but reasonable, value is adopted for the overshooting parameter, the stars do not become red supergiants during the PPI phase. We show that in this case most of the hydrogen envelope remains after the mass ejection by PPI. We find that the BH mass could be at most around 110 M-circle dot below the mass range of pair-instability supernovae.
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