  We present new results for pulsating neutron stars. We have calculated the
eigenfrequencies of the modes that one would expect to be the most important
gravitational-wave sources: the fundamental fluid f-mode, the first pressure
p-mode and the first gravitational-wave w-mode, for twelve realistic equations
of state. From this numerical data we have inferred a set of ``empirical
relations'' between the mode-frequencies and the parameters of the star (the
radius R and the mass M). Some of these relation prove to be surprisingly
robust, and we show how they can be used to extract the details of the star
(radius, mass, eos) from observed modes with errors no larger than a few
percent.
