English
 
Help Privacy Policy Disclaimer
  Advanced SearchBrowse

Item

ITEM ACTIONSEXPORT
Add to Basket
  Local TagsRelease HistoryDetailsSummary

Released
Journal Article

Pulsational pair-instability and the mass gap of Population III Black Holes: Effects of overshooting

MPS-Authors
/persons/resource/persons245880

Takahashi,  Koh
Computational Relativistic Astrophysics, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

External Resource
No external resources are shared
Fulltext (restricted access)
There are currently no full texts shared for your IP range.
Fulltext (public)

2010.16032.pdf
(Preprint), 746KB

Supplementary Material (public)
There is no public supplementary material available
Citation

Umeda, H., Yoshida, T., Nagele, C., & Takahashi, K. (2020). Pulsational pair-instability and the mass gap of Population III Black Holes: Effects of overshooting. The Astrophysical Journal Letters, 905(2): L21. doi:10.3847/2041-8213/abcb96.


Cite as: https://hdl.handle.net/21.11116/0000-0007-A4FB-5
Abstract
Since the discovery of GW190521, several proposals have been put forward to
explain the formation of a black hole in the mass gap caused by (pulsational)
pair-instability, $M = 65-130 M_\odot$. We calculate the mass ejection of Pop
III stars by the pulsational pair-instability (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 super
giants 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 $M = 109 M_\odot$ below the mass range of pair-instability
supernovae.