Chirp Mass and Spin of Binary Black Holes from First Star Remnants

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 $M_{\mathrm{chirp}}\sim 30M_{\odot }$ 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 $/yr/Gp{\mathrm{c}}^3$ which is consistent with the aLIGO/aVIRGO result of 9.7--101 $/yr/Gp{\mathrm{c}}^3$. 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 $⟨{\chi }_{\mathrm{eff}}⟩$ 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.

comments welcome. Accepted by MNRAS

References in corpus (5)

• Binary interaction dominates the evolution of massive stars
• The Mass Spectrum of the First Stars
• Effects of rotation on the evolution of primordial stars
• Double-core evolution and the formation of neutron-star binaries with compact companions
• How to confirm the existence of population III stars by observations of gravitational waves

Cited by in corpus (5)

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• Dynamical evolution of Population III stellar systems and the resulting binary statistics
• On the population III binary black hole mergers beyond the pair-instability mass gap
• Gravitational waves from the remnants of the first stars in nuclear star clusters
• An eccentric binary blackhole in post-Newtonian theory