Dataset Open Access

How loud are neutron star mergers?

Bernuzzi, Sebastiano; Radice, David; Ott, Christian D.; Roberts, Luke F.; Mösta, Philipp; Galeazzi, Filippo

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

Files (107.5 MB)
Name Size
DD2_M135135_D40_LK_Z4c.tar.gz
md5:ad59dcf2aafebd87a469dfce13bfff1d
5.8 MB Download
DD2_M135135_D40_LK_Z4c_HR.tar.gz
md5:d3d61246fd826ffa68279f83613c3ad2
5.6 MB Download
DD2_M1365125_D40_LK_Z4c.tar.gz
md5:99453b36b30b718677778aff5cb23f2e
6.3 MB Download
DD2_M1365125_D40_LK_Z4c_HR.tar.gz
md5:3cb7c6be848e7b993634a32f036c7358
4.9 MB Download
DD2_M140120_D40_LK_Z4c.tar.gz
md5:ad3659ff8914c9aa60ef73149875e0b4
5.5 MB Download
DD2_M140120_D40_LK_Z4c_HR.tar.gz
md5:e6677455965258551f95bb8009df2be6
5.2 MB Download
DD2_M144139_D40_LK_Z4c.tar.gz
md5:37428285adb528a6ee6072c49e5bdba0
5.1 MB Download
DD2_M144139_D40_LK_Z4c_HR.tar.gz
md5:2ec3f7d34778ec08ecd0e1e424b0f674
5.4 MB Download
LS220_M135135_D40_LK_Z4c.tar.gz
md5:743f8274ee7400a539a02f243064d779
5.1 MB Download
LS220_M135135_D40_LK_Z4c_HR_v2.tar.gz
md5:66e4d149b03b93c001778d8e0f1464fe
4.5 MB Download
LS220_M1365125_D40_LK_Z4c.tar.gz
md5:a6d13d9679786586e8e3e5706e2a8c2a
5.7 MB Download
LS220_M1365125_D40_LK_Z4c_HR_v2.tar.gz
md5:4137cfab7082431e6ec8f93589904f4a
5.6 MB Download
LS220_M140120_D40_LK_Z4c.tar.gz
md5:4438f89771640d80299c85b46d4a4724
5.6 MB Download
LS220_M140120_D40_LK_Z4c_HR.tar.gz
md5:44f9226ed4ba6cbc9a4337d3f217cb24
4.4 MB Download
LS220_M144139_D40_LK_Z4c.tar.gz
md5:82d0dc7aa0f45f30428207dcc172ba81
1.5 MB Download
LS220_M144139_D40_LK_Z4c_HR.tar.gz
md5:8064e648785d0172304423dad0d31766
3.3 MB Download
SFHo_M135135_D40_LK_Z4c.tar.gz
md5:97546b0c641d7fb399b2742408f7851f
1.8 MB Download
SFHo_M135135_D40_LK_Z4c_HR.tar.gz
md5:c2c72cf8faa6ce888511769abd1946f2
2.7 MB Download
SFHo_M1365125_D40_LK_Z4c.tar.gz
md5:5b53ea3ef7bab9310264a9214fe8290d
5.4 MB Download
SFHo_M1365125_D40_LK_Z4c_HR.tar.gz
md5:13ff67934e21bb6a66a3cebe5bebfbf6
4.1 MB Download
SFHo_M140120_D40_LK_Z4c.tar.gz
md5:3d07842bfa35ba5b3d876bc48bf1cfc3
5.4 MB Download
SFHo_M140120_D40_LK_Z4c_HR.tar.gz
md5:20d6d24b444e1ce042df817501fc90ac
4.8 MB Download
SFHo_M144139_D40_LK_Z4c.tar.gz
md5:71b92d3f8c31b4fcefa23d3268d82f32
1.9 MB Download
SFHo_M144139_D40_LK_Z4c_HR.tar.gz
md5:eb98eb21cd7018c570a148209f4cbfe8
1.8 MB Download
  • How loud are neutron star mergers? Sebastiano Bernuzzi, David Radice, Christian D. Ott, Luke F. Roberts, Philipp Mösta, and Filippo Galeazzi, Phys. Rev. D 94, 024023, 2016. http://arxiv.org/abs/1512.06397
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