  Models of thermal emission of neutron stars, presumably formed in their
atmospheres, are needed to infer the surface temperatures, magnetic fields,
chemical composition, and neutron star masses and radii from the observational
data. This information, supplemented with model equations of state and neutron
star cooling models, is expected to move us further in understanding the
fundamental properties of the superdense matter in the neutron star interiors.
The neutron star atmospheres are very different from those of usual stars due
to the immense gravity and huge magnetic fields. In this presentation we review
the current status of the neutron star atmosphere modeling and present most
important results.
