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Glitches -- sudden increases in spin rate -- are observed in many pulsars.One mechanism advanced to explain glitches in the youngest pulsars is that theyare caused by a starquake, a sudden rearrangement of the crust of the neutronstar. Starquakes have the potential to excite some of the oscillation modes ofthe neutron star, which means that they are of interest as a source ofgravitational waves. These oscillations could also have an impact on radioemission. In this paper we make upper estimates of the amplitude of theoscillations produced by a starquake, and the corresponding gravitational waveemission. We then develop a more detailed framework for calculating theoscillations excited by the starquake, using a toy model of a solid,incompressible star where all strain is lost instantaneously from the star atthe glitch. For this toy model, we give plots of the amplitudes of the modesexcited, as the shear modulus and rotation rate of the star are varied. We findthat for our specific model, the largest excitation is generally of a modesimilar to the $f$-mode of an incompressible fluid star, but that other modesof the star are excited to a significant degree over small parameter ranges ofthe rotation rate.

Developing a model for neutron star oscillations following starquakes