Towards Gravitational Wave Signals from Realistic Core Collapse Supernova Models

Kavli Affiliate: David H. Shoemaker

| First 5 Authors: Ewald Mueller, Markus Rampp, Robert Buras, H. -Thomas Janka, David H. Shoemaker

| Summary:

We have computed the gravitational wave signal from supernova core collapse
using the presently most realistic input physics available. We start from
state-of-the-art progenitor models of rotating and non-rotating massive stars,
and simulate the dynamics of their core collapse by integrating the equations
of axisymmetric hydrodynamics together with the Boltzmann equation for the
neutrino transport including an elaborate description of neutrino interactions,
and a realistic equation of state. We compute the quadrupole wave amplitudes,
the Fourier wave spectra, the amount of energy radiated in form of
gravitational waves, and the S/N ratios for the LIGO and the tuned Advanced
LIGO interferometers resulting both from non-radial mass motion and anisotropic
neutrino emission. The simulations demonstrate that the dominant contribution
to the gravitational wave signal is produced by neutrino-driven convection
behind the supernova shock. For stellar cores rotating at the extreme of
current stellar evolution predictions, the core-bounce signal is detectable
with advanced LIGO up to a distance of 5kpc, whereas the signal from post-shock
convection is observable up to a distance of about 100kpc. If the core is
non-rotating its gravitational wave emission can be measured up to a distance
of 15kpc, while the signal from the Ledoux convection in the deleptonizing,
nascent neutron star can be detected up to a distance of 10kpc. Both kinds of
signals are generically produced by convection in any core collapse supernova.

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