Gravitational waves from newly born, hot neutron stars

Details Gravitational waves from newly born, hot neutron stars Gravitational waves from newly born, hot neutron stars

2002-10-26

arxiv.org/abs/astro-ph/0210581v2

Mon.Not.Roy.Astron.Soc.342:629,2003

Astronomy and Astrophysics

Astrophysics

Minor changes in Section 4.1, Table 3 and Figure 5. Accepted for publication in MNRAS

Scientific paper

10.1046/j.1365-8711.2003.06580.x

We study the gravitational radiation associated to the non--radial oscillations of newly born, hot neutron stars. The frequencies and damping times of the relevant quasi--normal modes are computed for two different models of proto--neutron stars, at different times of evolution, from its birth until it settles down as a cold neutron star. We find that the oscillation properties of proto--neutron stars are remarkably different from those of their cold, old descendants and that this affects the characteristic features of the gravitational signal emitted during the post-collapse evolution. The consequences on the observability of these signals by resonant--mass and interferometric detectors are analyzed. We find that gravitational waves from the pulsations of a newborn proto--neutron star in the galaxy could be detected with a signal to noise ratio of 5 by the first generation interferometers, if the energy stored in the modes is greater than $\sim 10^{-8} M_\odot c^2$, or by a resonant antenna if it is greater than $\sim 10^{-4} M_\odot c^2$. In addition since at early times the frequency of the spacetime modes is much lower than that of a cold neutron star, they would be also detectable with the same signal to noise ratio if a comparable amount of energy is radiated into these modes.

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