How loud are neutron star mergers?

We release neutron star merger waveforms computed using fully general relativistic simulations of equal and unequal-mass binaries drawn from the galactic population. The simulations employ finite-temperature microphysical equations of state (LS220, DD2, and SFHo) and neutrino cooling. Please, see

http://arxiv.org/abs/1512.06397

for details.

Each tarball refers to a simulation and contains

• Curvature multipolar waveform \(\psi^{(4)}_{\ell m}\)
• Metric multipolar waveform \(h_{\ell m}\)
• Radiated energy and angular momentum

Files:

• waveforms/Psi4_l?_m?_r200.txt
  • Columns: \(t,\ \Re{(\psi^{(4)}_{\ell m})},\ \Im{(\psi^{(4)}_{\ell m})} \)
• waveforms/Rh_l?_m?_r200.txt
  • Columns: \(u/M,\ \Re{(h_{\ell m})}/M,\ \Im{(h_{\ell m})}/M,\ \Re{(\dot{h}_{\ell m})},\ \Im{(\dot{h}_{\ell m}}),\ M\omega_{\ell m},\ A_{\ell m}/M,\ \phi_{\ell m},\ t \)
• waveforms/Ej_r200.txt
  • Columns: \(E_b,\ j,\ E_\text{rad},\ J_\text{rad},\ t \)

where

• \(t\) simulation time
• \(u\) retarded time
• \(M\) binary mass
• \(\omega_{\ell m}\) wave frequency
• \(A_{\ell m}\) wave amplitude
• \(\phi_{\ell m}\) wave phase
• \(E_\text{GW}\) radiated energy
• \(J_\text{GW}\) radiated angular momentum
• \(E_b\) binary energy
• \(j\) binary specific angular momentum

Please refer to the paper and references therein for the definition of the different quantities.

Units \(c=G=M_\text{Sun}=1\)