Resumen de Stellar Perturbations
In this chapter the theory of non-rotating perfect fluid stellar adiabatic perturbations is derived in a similar way to black hole perturbations. In that case a wave equation can be obtained only for the axial perturbations. Whereas for black holes quasi-normal modes are purely gravitational, the modes of oscillation of stars are due to the coupling between the fluid and the gravitational field. This means that the emitted radiation carries information on the structure of the source.
