  Astrophysical observations of compact stars provide, in addition to collider
experiments, the other big source of information on matter under extreme
conditions. The largest and most precise data set about neutron stars is the
timing data of radio pulsars. We show how this unique data can be used to learn
about the ultra-dense matter in the compact star interior. The method relies on
astro-seismology based on special global oscillation modes (r-modes) that emit
gravitational waves. They would prevent pulsars from spinning with their
observed high frequencies, unless the damping of these modes, determined by the
microscopic properties of matter, can prevent this. We show that for each form
of matter there is a distinct region in a frequency/spindown-rate diagram where
r-modes can be present. We find that stars containing ungapped quark matter are
consistent with both the observed radio and x-ray data, whereas, even when
taking into account the considerable uncertainties, neutron star models with
standard viscous damping are inconsistent with both data sets and additional
damping mechanisms would be required.
