Gravitational waves from very massive stars collapsing to a black hole
Abstract
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 320 M⊙ and ≈150 M⊙, 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 ≲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 ≳300 M⊙ and their pair-unstable collapse in the Universe.
- Publication:
-
Physical Review D
- Pub Date:
- February 2019
- DOI:
- 10.1103/PhysRevD.99.041302
- Bibcode:
- 2019PhRvD..99d1302U