Universal relation for supernova gravitational waves. (arXiv:2110.03131v3 [astro-ph.HE] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Sotani_H/0/1/0/all/0/1">Hajime Sotani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Takiwaki_T/0/1/0/all/0/1">Tomoya Takiwaki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Togashi_H/0/1/0/all/0/1">Hajime Togashi</a>
Using the numerical simulation data for two-dimensional core-collapse
supernova, we examine the protoneutron star (PNS) asteroseismology with the
relativistic Cowling approximation. As shown in the previous study, the
gravitational wave signals appearing in the numerical simulation can be well
identified with the gravity (fundamental) oscillation in the early (later)
phase before (after) the avoided crossing between the gravity and fundamental
oscillations. On the other hand, the time evolution of supernova gravitational
waves strongly depends on the PNS models, such as the progenitor mass and the
equation of state for dense matter. Nevertheless, we find that the fundamental
and gravity mode frequencies according to the gravitational wave signals
appearing in the numerical simulations can be expressed as a function of the
protoneutron star average density independently of the PNS models. Using the
average density, we derive the empirical formula for supernova gravitational
wave frequency. In addition, we confirm that the dependence of the PNS surface
density on the PNS average density is almost independent of the PNS models and
also discuss how the different treatment of the non-uniform matter in the
equation of state affects the observables.
Using the numerical simulation data for two-dimensional core-collapse
supernova, we examine the protoneutron star (PNS) asteroseismology with the
relativistic Cowling approximation. As shown in the previous study, the
gravitational wave signals appearing in the numerical simulation can be well
identified with the gravity (fundamental) oscillation in the early (later)
phase before (after) the avoided crossing between the gravity and fundamental
oscillations. On the other hand, the time evolution of supernova gravitational
waves strongly depends on the PNS models, such as the progenitor mass and the
equation of state for dense matter. Nevertheless, we find that the fundamental
and gravity mode frequencies according to the gravitational wave signals
appearing in the numerical simulations can be expressed as a function of the
protoneutron star average density independently of the PNS models. Using the
average density, we derive the empirical formula for supernova gravitational
wave frequency. In addition, we confirm that the dependence of the PNS surface
density on the PNS average density is almost independent of the PNS models and
also discuss how the different treatment of the non-uniform matter in the
equation of state affects the observables.
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