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Abstract

Short duration GRBs (SGRBs) are widely believed to be powered by the mergers of compact binaries, like binary neutron stars or possibly neutron star-black hole binaries. Though the prospect of detecting SGRBs with gravitational wave (GW) signals by the advanced LIGO/VIRGO network is promising, no known SGRB has been found within the expected advanced LIGO/VIRGO sensitivity range. We argue, however, that the two long-short GRBs (GRB 060505 and GRB 060614) may be within the horizon of advanced GW detectors. In the upcoming era of GW astronomy, the merger origin of some long-short GRBs, as favored by the macronova signature displayed in GRB 060614, can be unambiguously tested. The model-dependent time-lags between the merger and the onset of the prompt emission of GRB are estimated. The comparison of such time-lags between model prediction to the real data expected in the era of the GW astronomy would be helpful in revealing the physical processes taking place at the central engine (including the launch of the relativistic outflow, the emergence of the outflow from the dense material ejected during the merger and the radiation of gamma-rays). The achievable accuracy of measuring the speed of GW in the advanced LIGO/VIRGO era is also examined.