Features of Accretion Phase Gravitational Wave Emission from Two-dimensional Rotating Core-Collapse Supernovae. (arXiv:1901.09055v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Pajkos_M/0/1/0/all/0/1">Michael A. Pajkos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Couch_S/0/1/0/all/0/1">Sean M. Couch</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pan_K/0/1/0/all/0/1">Kuo-Chuan Pan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+OConnor_E/0/1/0/all/0/1">Evan P. O'Connor</a>
We explore the influence of progenitor mass and rotation on the gravitational
wave (GW) emission from core collapse supernovae, during the post bounce, pre
explosion, accretion phase. We present the results from 15 two-dimensional (2D)
neutrino radiation-hydrodynamic simulations from initial stellar collapse to
$sim$300 ms after core bounce. We examine the features of the GW signals for
four zero age main sequence (ZAMS) progenitor masses ranging from 12 $M_odot$
to 60 $M_odot$ and four core rotation rates from 0 rad s$^{-1}$ to 3 rad
s$^{-1}$. We find that GW strain immediately around core bounce is fairly
independent of ZAMS mass and—consistent with previous findings—that it is
more heavily dependent on the core angular momentum. At later times, all
nonrotating progenitors exhibit loud GW emission, which we attribute to
vibrational g-modes of the protoneutron star excited by convection in the post
shock layer and the standing accretion shock instability (SASI). We find that
increasing rotation rates results in muting of the accretion phase GW signal
due to centrifugal effects that inhibit convection in the post shock region,
quench the SASI, and slow the rate at which the protoneutron star peak
vibrational frequency increases. Additionally, we verify the efficacy of our
approximate general relativistic (GR) effective potential treatment of gravity
by comparing our core bounce GW strains with the recent 2D GR results of other
groups.
We explore the influence of progenitor mass and rotation on the gravitational
wave (GW) emission from core collapse supernovae, during the post bounce, pre
explosion, accretion phase. We present the results from 15 two-dimensional (2D)
neutrino radiation-hydrodynamic simulations from initial stellar collapse to
$sim$300 ms after core bounce. We examine the features of the GW signals for
four zero age main sequence (ZAMS) progenitor masses ranging from 12 $M_odot$
to 60 $M_odot$ and four core rotation rates from 0 rad s$^{-1}$ to 3 rad
s$^{-1}$. We find that GW strain immediately around core bounce is fairly
independent of ZAMS mass and—consistent with previous findings—that it is
more heavily dependent on the core angular momentum. At later times, all
nonrotating progenitors exhibit loud GW emission, which we attribute to
vibrational g-modes of the protoneutron star excited by convection in the post
shock layer and the standing accretion shock instability (SASI). We find that
increasing rotation rates results in muting of the accretion phase GW signal
due to centrifugal effects that inhibit convection in the post shock region,
quench the SASI, and slow the rate at which the protoneutron star peak
vibrational frequency increases. Additionally, we verify the efficacy of our
approximate general relativistic (GR) effective potential treatment of gravity
by comparing our core bounce GW strains with the recent 2D GR results of other
groups.
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