How loud are neutron star mergers?
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下载链接：
https://zenodo.org/records/57844
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资源简介：
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 \(c=G=M_\text{Sun}=1\)
创建时间：
2020-01-24
