Abstract
The amount of gravitational radiation predicted by numerical calculations of the collapse of rotating stellar cores is reviewed. As far as axisymmetric models are concerned there has been a significant improvement of the models within the last few years. The improvement of the models, however, was accompanied by more and more reduced predictions of the total energy radiated in form of gravitational waves, the most realistic models suggesting an energy loss of the order 10-6M⊙c2. For a source situated at a distance of 10Mpc (≈Virgo Cluster) the corresponding (dimensionless) wave amplitude h is smaller than 10-22, which seems to be even beyond the realm of the third generation gravitational wave detectors. On the other hand non-axisymmetric models predict up to 100 times larger radiative efficiencies. Unfortunately both classes of models still have common shortcomings due to uncertainties in the equation of state,due to the unknown initial model and due to the final fate of the collapsing cores.
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Müller, E. (1984). The Collapse of Rotating Stellar Cores: The Amount of Gravitational Radiation Predicted By Various Numerical Models. In: Bancel, D., Signore, M. (eds) Problems of Collapse and Numerical Relativity. NATO ASI Series, vol 134. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-6460-0_19
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