  We present two frameworks to infer some of the properties of neutron stars
from their electromagnetic radiation and the emission of continuous
gravitational waves due to r-mode oscillations. In the first framework,
assuming a distance measurement via electromagnetic observations, we infer
three neutron star properties: the moment of inertia, a parameter related to
the r-mode saturation amplitude, and the component of magnetic dipole moment
perpendicular to the rotation axis. Unlike signals from mountains, r-mode
oscillations provide additional information through a parameter (\kappa) that
satisfies a universal relation with the star's compactness. In the second
framework, we utilize this and the relation between the moment of inertia and
compactness, in addition to assuming an equation of state and utilizing pulsar
frequency measurements, to directly measure the neutron star's distance along
with the aforementioned parameters. We employ a Fisher information matrix-based
approach for quantitative error estimation in both frameworks. We find that the
error in the distance measurement dominates the errors in the first framework
for any reasonable observation time. In contrast, due to the low errors in
pulsar frequency measurements, parameters can be inferred accurately via the
second framework but work only in a restricted parameter space. We finally
address potential ways to overcome critical drawbacks of our analyses and
discuss directions for future work.
