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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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    <subfield code="a">&lt;p&gt;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&lt;/p&gt;

&lt;p&gt;http://arxiv.org/abs/1512.06397&lt;/p&gt;

&lt;p&gt;for details.&lt;/p&gt;

&lt;p&gt;&amp;nbsp;&lt;/p&gt;

&lt;p&gt;Each tarball refers to a simulation and contains&lt;/p&gt;

&lt;ul&gt;
	&lt;li&gt;Curvature multipolar waveform &lt;span class="math-tex"&gt;\(\psi^{(4)}_{\ell m}\)&lt;/span&gt;&lt;/li&gt;
	&lt;li&gt;Metric multipolar waveform &lt;span class="math-tex"&gt;\(h_{\ell m}\)&lt;/span&gt;&lt;/li&gt;
	&lt;li&gt;Radiated energy and angular momentum&lt;/li&gt;
&lt;/ul&gt;

&lt;p&gt;Files:&lt;/p&gt;

&lt;ul&gt;
	&lt;li&gt;&lt;em&gt;waveforms/Psi4_l?_m?_r200.txt &lt;/em&gt;

	&lt;ul&gt;
		&lt;li&gt;Columns: &lt;span class="math-tex"&gt;\(t,\ \Re{(\psi^{(4)}_{\ell m})},\ \Im{(\psi^{(4)}_{\ell m})} \)&lt;/span&gt;&lt;/li&gt;
	&lt;/ul&gt;
	&lt;/li&gt;
	&lt;li&gt;&lt;em&gt;waveforms/Rh_l?_m?_r200.txt&lt;/em&gt;
	&lt;ul&gt;
		&lt;li&gt;Columns: &lt;span class="math-tex"&gt;\(u/M,\ \Re{(h_{\ell m})}/M,\ \Im{(h_{\ell m})}/M,\ \Re{(\dot{h}_{\ell m})},\ \Im{(\dot{h}_{\ell m}}),\ M\omega_{\ell m},\ A_{\ell m}/M,\ \phi_{\ell m},\ t \)&lt;/span&gt;&lt;/li&gt;
	&lt;/ul&gt;
	&lt;/li&gt;
	&lt;li&gt;&lt;em&gt;waveforms/Ej_r200.txt&lt;/em&gt;
	&lt;ul&gt;
		&lt;li&gt;Columns: &lt;span class="math-tex"&gt;\(E_b,\ j,\ E_\text{rad},\ J_\text{rad},\ t \)&lt;/span&gt;&lt;/li&gt;
	&lt;/ul&gt;
	&lt;/li&gt;
&lt;/ul&gt;

&lt;p&gt;where&lt;/p&gt;

&lt;ul&gt;
	&lt;li&gt;&lt;span class="math-tex"&gt;\(t\)&lt;/span&gt; simulation time&lt;/li&gt;
	&lt;li&gt;&lt;span class="math-tex"&gt;\(u\)&lt;/span&gt; retarded time&lt;/li&gt;
	&lt;li&gt;&lt;span class="math-tex"&gt;\(M\)&lt;/span&gt; binary mass&lt;/li&gt;
	&lt;li&gt;&lt;span class="math-tex"&gt;\(\omega_{\ell m}\)&lt;/span&gt; wave frequency&lt;/li&gt;
	&lt;li&gt;&lt;span class="math-tex"&gt;\(A_{\ell m}\)&lt;/span&gt; wave amplitude&lt;/li&gt;
	&lt;li&gt;&lt;span class="math-tex"&gt;\(\phi_{\ell m}\)&lt;/span&gt; wave phase&lt;/li&gt;
	&lt;li&gt;&lt;span class="math-tex"&gt;\(E_\text{GW}\)&lt;/span&gt; radiated energy&lt;/li&gt;
	&lt;li&gt;&lt;span class="math-tex"&gt;\(J_\text{GW}\)&lt;/span&gt; radiated angular momentum&lt;/li&gt;
	&lt;li&gt;&lt;span class="math-tex"&gt;\(E_b\)&lt;/span&gt; binary energy&lt;/li&gt;
	&lt;li&gt;&lt;span class="math-tex"&gt;\(j\)&lt;/span&gt; binary specific angular momentum&lt;/li&gt;
&lt;/ul&gt;

&lt;p&gt;Please refer to the paper and references therein for the definition of the different quantities.&lt;/p&gt;

&lt;p&gt;Units &lt;span class="math-tex"&gt;\(c=G=M_\text{Sun}=1\)&lt;/span&gt;&lt;/p&gt;</subfield>
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