Help Privacy Policy Disclaimer
  Advanced SearchBrowse




Journal Article

Gravitational waves from very massive stars collapsing to a black hole


Shibata,  Masaru
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)

(Preprint), 242KB

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

Uchida, H., Shibata, M., Takahashi, K., & Yoshida, T. (2019). Gravitational waves from very massive stars collapsing to a black hole. Physical Review D, 99(4): 041302. doi:10.1103/PhysRevD.99.041302.

Cite as: https://hdl.handle.net/21.11116/0000-0003-023D-7
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 $\approx 150M_\odot$, respectively. We find that
for the moderately rapidly rotating cases, the peak strain amplitude and the
corresponding frequency of gravitational waves are $\sim 10^{-22}$ and $f
\approx 300$--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 $D
\sim 100$~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.