Figure 26: The GW signal from convection in a proto neutron star. The top panel shows the GW
quadrupole amplitude as a function of time for both the convective mass flow (thick line) and
anisotropic neutrino emission (thin line). The combined spectral energy distribution of the quadrupole
radiation for both sources is shown in the middle figure, with just the neutrino component alone in
the bottom panel. Note that although the quadrupole amplitude for the neutrino emission is much
higher, it varies slower than the mass motions. Hence, it only dominates the signal at low frequencies.
(Figures from [209]; used with permission.)
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