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We explore the influence of progenitor mass and rotation on thegravitational-wave (GW) emission from core-collapse supernovae, during thepostbounce, preexplosion, accretion-phase. We present the results from 15two-dimensional (2D) neutrino radiation-hydrodynamic simulations from initialstellar collapse to $\sim$300 ms after core bounce. We examine the features ofthe GW signals for four zero-age main sequence (ZAMS) progenitor masses rangingfrom 12 $M_\odot$ to 60 $M_\odot$ and four core rotation rates from 0 to 3 rads$^{-1}$. We find that GW strain immediately around core bounce is fairlyindependent of ZAMS mass and---consistent with previous findings---that it ismore heavily dependent on the core angular momentum. At later times, allnonrotating progenitors exhibit loud GW emission, which we attribute tovibrational g-modes of the protoneutron star (PNS) excited by convection in thepostshock layer and the standing accretion shock instability (SASI). We findthat increasing rotation rates results in muting of the accretion-phase GWsignal due to centrifugal effects that inhibit convection in the postshockregion, quench the SASI, and slow the rate at which the PNS peak vibrationalfrequency increases. Additionally, we verify the efficacy of our approximategeneral relativistic (GR) effective potential treatment of gravity by comparingour core bounce GW strains with the recent 2D GR results of other groups.

Features of Accretion-phase Gravitational-wave Emission from Two-dimensional Rotating Core-collapse Supernovae