  The detection of gravitational wave events has stimulated theoretical
modeling of the formation and evolution of double compact objects (DCOs).
However, even for the most studied isolated binary evolution channel, there
exist large uncertainties in the input parameters and treatments of the binary
evolution process. So far, double neutron stars (DNSs) are the only DCOs for
which direct observations are available through traditional electromagnetic
astronomy. In this work, we adopt a population synthesis method to investigate
the formation and evolution of Galactic DNSs. We construct 324 models for the
formation of Galactic DNSs, taking into account various possible combinations
of critical input parameters and processes such as mass transfer efficiency,
supernova type, common envelope efficiency, neutron star kick velocity, and
pulsar selection effect. We employ Bayesian analysis to evaluate the adopted
models by comparing with observations. We also compare the expected DNS merger
rate in the Galaxy with that inferred from the known Galactic population of
Pulsar-NS systems. Based on these analyses we derive favorable range of the
aforementioned key parameters.
