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Abridged: Using a suite of progenitor models, neutrino luminosities, and two-dimensional (2D) simulations, we investigate the matter gravitational-wave (GW)emission from postbounce phases of neutrino-driven core-collapse supernovae(CCSNe). The relevant phases are prompt and steady-state convection, thestanding accretion shock instability (SASI), and asymmetric explosions. For thestages before explosion, we propose a model for the source of GW emission.Downdrafts of the postshock-convection/SASI region strike the protoneutron star"surface" with large speeds and are decelerated by buoyancy forces. We findthat the GW amplitude is set by the magnitude of deceleration and, byextension, the downdraft's speed and the vigor of postshock-convective/SASImotions. However, the characteristic frequencies, which evolve from ~100 Hzafter bounce to ~300-400 Hz, are primarily independent of these speeds, but areset by the deceleration timescale, which is in turn set by the buoyancyfrequency at the lower boundary of postshock convection. Consequently, the GWcharacteristic frequencies are dependent upon a combination of core structureattributes, specifically the dense-matter equation of state (EOS) and detailsthat determine the gradients at the boundary, including the accretion-ratehistory, the EOS at subnuclear densities, and neutrino transport. Duringexplosion, the high frequency signal wanes and is replaced by a strong lowfrequency, ~10s of Hz, signal that reveals the general morphology of theexplosion (i.e. prolate, oblate, or spherical). However, current andnear-future GW detectors are sensitive to GW power at frequencies >50 Hz.Therefore, the signature of explosion will be the abrupt reduction ofdetectable GW emission.

A Model for Gravitational Wave Emission from Neutrino-Driven Core-Collapse Supernovae