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Chirp Mass and Spin of Binary Black Holes from First Star Remnants
- Publication Year :
- 2020
- Publisher :
- arXiv, 2020.
-
Abstract
- We performed Population III (Pop III) binary evolution by using population synthesis simulations for seven different models. We found that Pop III binaries tend to be binary black holes (BBHs) with chirp mass $M_{\rm chirp} \sim 30~M_{\odot}$ and they can merge at present day due to long merger time. The merger rate densities of Pop III BBHs at $z=0$ ranges 3.34--21.2 $\rm /yr/Gpc^3$ which is consistent with the aLIGO/aVIRGO result of 9.7--101 $\rm /yr/Gpc^3$. These Pop III binaries might contribute to some part of the massive BBH gravitational wave (GW) sources detected by aLIGO/aVIRGO. We also calculated the redshift dependence of Pop III BBH mergers. We found that Pop III low spin BBHs tend to merge at low redshift, while Pop III high spin BBHs do at high redshift, which can be confirmed by future GW detectors such as ET, CE, and DECIGO. These detectors can also check the redshift dependence of BBH merger rate and spin distribution. Our results show that except for one model, the mean effective spin $\left\langle \chi_{\rm eff} \right\rangle$ at $z=0$ ranges $0.02$--$0.3$ while at $z=10$ it does $0.16$--$0.64$. Therefore, massive stellar-mass BBH detection by GWs will be a key for the stellar evolution study in the early universe.<br />Comment: comments welcome. Accepted by MNRAS
- Subjects :
- Physics
High Energy Astrophysical Phenomena (astro-ph.HE)
education.field_of_study
Gravitational wave
Population
Binary number
FOS: Physical sciences
Astronomy and Astrophysics
Astrophysics
Redshift
Astrophysics - Solar and Stellar Astrophysics
Binary black hole
Space and Planetary Science
Chirp
Population synthesis
Astrophysics - High Energy Astrophysical Phenomena
education
Stellar evolution
Solar and Stellar Astrophysics (astro-ph.SR)
Subjects
Details
- Database :
- OpenAIRE
- Accession number :
- edsair.doi.dedup.....f386871853967e7bb22d21faa3101809
- Full Text :
- https://doi.org/10.48550/arxiv.2005.09795