Gravitational-wave signal of a core-collapse supernova explosion of a 15 Solar mass star. (arXiv:2007.15099v1 [astro-ph.HE])

Gravitational-wave signal of a core-collapse supernova explosion of a 15 Solar mass star. (arXiv:2007.15099v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Mezzacappa_A/0/1/0/all/0/1">Anthony Mezzacappa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marronetti_P/0/1/0/all/0/1">Pedro Marronetti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Landfield_R/0/1/0/all/0/1">Ryan E. Landfield</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lentz_E/0/1/0/all/0/1">Eric J. Lentz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yakunin_K/0/1/0/all/0/1">Konstantin N. Yakunin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bruenn_S/0/1/0/all/0/1">Stephen W. Bruenn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hix_W/0/1/0/all/0/1">W. Raphael Hix</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Messer_O/0/1/0/all/0/1">O.E. Bronson Messer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Endeve_E/0/1/0/all/0/1">Eirik Endeve</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blondin_J/0/1/0/all/0/1">John M. Blondin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Harris_J/0/1/0/all/0/1">J. Austin Harris</a>

We report on the gravitational wave signal computed in the context of a
three-dimensional simulation of a core collapse supernova explosion of a 15
Solar mass star. The simulation was performed with our neutrino hydrodynamics
code Chimera. We detail the gravitational wave strains as a function of time,
for both polarizations, and discuss their physical origins. We also present the
corresponding spectral signatures. Gravitational wave emission in our model has
two key features: low-frequency emission (< 200 Hz) emanates from the gain
layer as a result of neutrino-driven convection and the SASI and high-frequency
emission (> 600 Hz) emanates from the proto-neutron star due to Ledoux
convection within it. The high-frequency emission dominates the gravitational
wave emission in our model and emanates largely from the convective layer
itself, not from the convectively stable layer above it, due to convective
overshoot. Moreover, the low-frequency emission emanates from the gain layer
itself, not from the proto-neutron star, due to accretion onto it. We provide
evidence of the SASI in our model and demonstrate that the peak of our
low-frequency gravitational wave emission spectrum corresponds to it. Given its
origin in the gain layer, we classify the SASI emission in our model as p-mode
emission and assign a purely acoustic origin, not a vortical-acoustic origin,
to it. Our dominant proto-neutron star gravitational wave emission is not well
characterized by emission from surface g-modes, complicating the relationship
between peak frequencies observed and the mass and radius of the proto-neutron
star expressed by analytic estimates under the assumption of surface g-mode
emission. We present our frequency normalized characteristic strain along with
the sensitivity curves of current- and next-generation gravitational wave
detectors.

We report on the gravitational wave signal computed in the context of a
three-dimensional simulation of a core collapse supernova explosion of a 15
Solar mass star. The simulation was performed with our neutrino hydrodynamics
code Chimera. We detail the gravitational wave strains as a function of time,
for both polarizations, and discuss their physical origins. We also present the
corresponding spectral signatures. Gravitational wave emission in our model has
two key features: low-frequency emission (< 200 Hz) emanates from the gain
layer as a result of neutrino-driven convection and the SASI and high-frequency
emission (> 600 Hz) emanates from the proto-neutron star due to Ledoux
convection within it. The high-frequency emission dominates the gravitational
wave emission in our model and emanates largely from the convective layer
itself, not from the convectively stable layer above it, due to convective
overshoot. Moreover, the low-frequency emission emanates from the gain layer
itself, not from the proto-neutron star, due to accretion onto it. We provide
evidence of the SASI in our model and demonstrate that the peak of our
low-frequency gravitational wave emission spectrum corresponds to it. Given its
origin in the gain layer, we classify the SASI emission in our model as p-mode
emission and assign a purely acoustic origin, not a vortical-acoustic origin,
to it. Our dominant proto-neutron star gravitational wave emission is not well
characterized by emission from surface g-modes, complicating the relationship
between peak frequencies observed and the mass and radius of the proto-neutron
star expressed by analytic estimates under the assumption of surface g-mode
emission. We present our frequency normalized characteristic strain along with
the sensitivity curves of current- and next-generation gravitational wave
detectors.

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