Gravitational Waves from Axisymmetric, Rotating Stellar Core Collapse

We have carried out an extensive set of two-dimensional, axisymmetric,purely-hydrodynamic calculations of rotational stellar core collapse with arealistic, finite-temperature nuclear equation of state and realistic massivestar progenitor models. For each of the total number of 72 differentsimulations we performed, the gravitational wave signature was extracted viathe quadrupole formula in the slow-motion, weak-field approximation. Weinvestigate the consequences of variation in the initial ratio of rotationalkinetic energy to gravitational potential energy and in the initial degree ofdifferential rotation. Furthermore, we include in our model suite progenitorsfrom recent evolutionary calculations that take into account the effects ofrotation and magnetic torques. For each model, we calculate gravitationalradiation wave forms, characteristic wave strain spectra, energy spectra, finalrotational profiles, and total radiated energy. In addition, we compare ourmodel signals with the anticipated sensitivities of the 1st- and 2nd-generationLIGO detectors coming on line. We find that most of our models are detectableby LIGO from anywhere in the Milky Way.Comment: 13 pages, 22 figures, accepted for publication in ApJ (v600, Jan. 2004). Revised version: Corrected typos and minor mistakes in text and references. Minor additions to the text according to the referee's suggestions, conclusions unchange