Gravitational waves and neutrino emission from the merger of binary neutron stars

Details Gravitational waves and neutrino emission from the merger of binary neutron stars Gravitational waves and neutrino emission from the merger of binary neutron stars

2011-05-11

arxiv.org/abs/1105.2125v2

Phys.Rev.Lett.107:051102,2011

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

4 pages, 4 figures (Fig.2 is in low resolution), Accepted for publication in PRL

Scientific paper

10.1103/PhysRevLett.107.051102

Numerical simulations for the merger of binary neutron stars are performed in full general relativity incorporating a finite-temperature (Shen's) equation of state (EOS) and neutrino cooling for the first time. It is found that for this stiff EOS, a hypermassive neutron star (HMNS) with a long lifetime ($\gg 10$ ms) is the outcome for the total mass $\alt 3.0M_{\odot}$. It is shown that the typical total neutrino luminosity of the HMNS is $\sim 3$--$8\times 10^{53}$ ergs/s and the effective amplitude of gravitational waves from the HMNS is 4--$6 \times 10^{-22}$ at $f=2.1$--2.5 kHz for a source distance of 100 Mpc. We also present the neutrino luminosity curve when a black hole is formed for the first time.

Affiliated with

Also associated with

No associations

Rating

Gravitational waves and neutrino emission from the merger of binary neutron stars does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Gravitational waves and neutrino emission from the merger of binary neutron stars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Gravitational waves and neutrino emission from the merger of binary neutron stars will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-611142