  In this paper we consider the population of eccentric binaries with a neutron
star and a white dwarf that has been revealed in our galaxy in recent years
through binary pulsar observations. We apply our statistical analysis method
(Kim, Kalogera, & Lorimer 2003)and calculate the Galactic formation rate of
these binaries empirically. We then compare our results with rate predictions
based on binary population synthesis from various research groups and for
various ranges of model input parameters. For our reference moel, we find the
Galactic formation rate of these eccentric systems to be ~7 per Myr, about an
order of magnitude smaller than results from binary evolution estimations.
However, the empirical estimates are calculated with no correction for pulsar
beaming, and therefore they should be taken as lower limits. Despite
uncertainties that exceed an order of magnitude, there is significant overlap
of the various rate calculations. This consistency lends confidence that our
current understanding of the formation of these eccentric NS-WD binaries is
reasonable.
