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Gamma-ray bursts (GRB) are the most powerful transient phenomena in theUniverse. Nowadays dozens of speculations on the origin of GRB were undertaken,but so far a single model for the origin of, in particular, short GRBs does notexist. The black hole (BH) - neutron star (NS) coalescence is a promisingcandidate source for short GRBs. Most of binary mergers numerical simulationswere carried out with the purpose of investigating the emission ofgravitational waves. Such a scenario consists of an inspiral, merging andringdown phase. In this paper we present the comparison of the observationalresults and analytical predictions for a test particle in a quasicircular orbitaround the BH. The emission of gravitational waves causes a rapid decrease ofthe orbital radius and a rise of a {\it chirp} of radiation. Matter orbitingthe black hole would be expected to produce high-frequency oscillations (HFO).Timescales of the coalescence process are of the order of milliseconds andoscillation frequencies of hundreds Hz for a system with a solar mass BHcompanion. We report on the detection of HFO in two short gamma-ray bursts inthis paper. The frequencies and durations of the oscillations are in agreementwith the predicted values. A {\it chirp} phenomenon is identified also. Wetherefore argue in favor of BH-NS mergers as a scenario for the production ofshort gamma-ray bursts.

The last stages of evolution of close binaries composed of compact companions