  Photospheric radius expansion during X-ray bursts can be used to measure
neutron star radii and help constrain the equation of state of neutron star
matter. Understanding the stellar wind dynamics is important for interpreting
observations. Stellar wind models, though studied in past decades, have thus
regained interest and need to be revisited with updated data and methods. In
this work we study the radiative wind model in the context of XRBs, with modern
techniques and physics input. We focus on characterization of the solutions and
study of observable magnitudes as a function of free model parameters. We
implement a spherically-symmetric non-relativistic wind model in a stationary
regime, with updated opacity tables and modern numerical techniques. Total mass
and energy outflows $(\dot M,\dot E)$ are treated as free parameters. A high
resolution parameter space exploration was performed to allow better
characterization of observable magnitudes. High correlation was found between
different photospheric magnitudes and free parameters. For instance, the
photospheric ratio of gravitational energy outflow to radiative luminosity is
in direct proportion to the photospheric wind velocity. The correlations found
could help determine the physical conditions of the inner layers, where nuclear
reactions take place, by means of observable photospheric values. Further
studies are needed to determine the range of physical conditions in which the
correlations are valid.
