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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