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How loud are neutron star mergers?

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

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<?xml version='1.0' encoding='utf-8'?>
<oai_dc:dc xmlns:dc="" xmlns:oai_dc="" xmlns:xsi="" xsi:schemaLocation="">
  <dc:creator>Bernuzzi, Sebastiano</dc:creator>
  <dc:creator>Radice, David</dc:creator>
  <dc:creator>Ott, Christian D.</dc:creator>
  <dc:creator>Roberts, Luke F.</dc:creator>
  <dc:creator>Mösta, Philipp</dc:creator>
  <dc:creator>Galeazzi, Filippo</dc:creator>
  <dc:description>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

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



		Columns: \(t,\ \Re{(\psi^{(4)}_{\ell m})},\ \Im{(\psi^{(4)}_{\ell m})} \)
		Columns: \(u/M,\ \Re{(h_{\ell m})}/M,\ \Im{(h_{\ell m})}/M,\ \Re{(\dot{h}_{\ell m})},\ \Im{(\dot{h}_{\ell m}}),\ M\omega_{\ell m},\ A_{\ell m}/M,\ \phi_{\ell m},\ t \)
		Columns: \(E_b,\ j,\ E_\text{rad},\ J_\text{rad},\ t \)


	\(t\) 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 \(c=G=M_\text{Sun}=1\)</dc:description>
  <dc:subject>Binary neutron stars</dc:subject>
  <dc:subject>Gravitational waves</dc:subject>
  <dc:subject>Numerical relativity</dc:subject>
  <dc:title>How loud are neutron star mergers?</dc:title>
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