2019/01/24 by Haruki Uchida, Masaru Shibata, Uchida, Haruki +5
Physics and Astronomy · #Astrophysical Phenomena and Observations #FOS: Physical sciences #Gamma-ray bursts and supernovae #High Energy Astrophysical Phenomena (astro-ph.HE) #Pulsars and Gravitational Waves Research #astro-ph.HE
paper · pdf · doi:10.48550/arxiv.1901.08260
5 pages, 3 figures, accepted to PRD
arxiv created 2019/01/24 · openalex publication_date 2019/01/24 · arxiv updated 2019/01/25 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We compute gravitational waves emitted by the collapse of a rotating very massive star (VMS) core leading directly to a black hole in axisymmetric numerical-relativity simulations. The evolved rotating VMS is derived by a stellar evolution calculation and its initial mass and the final carbon-oxygen core mass are 320M_\odot and ≈ 150M_\odot, respectively. We find that for the moderately rapidly rotating cases, the peak strain amplitude and the corresponding frequency of gravitational waves are ∼ 10-22 and f ≈ 300--600 Hz for an event at the distance of D=50~Mpc. Such gravitational waves will be detectable only for D \lesssim 10~Mpc by second generation detectors, advanced LIGO, advanced VIRGO, and KAGRA, even if the designed sensitivity for these detectors is achieved. However, third-generation detectors will be able to detect such gravitational waves for an event up to D ∼ 100~Mpc. The detection of the gravitational-wave signal will provide a potential opportunity for verifying the presence of VMSs with mass \gtrsim 300M_\odot and their pair-unstable collapse in the universe.