  The Doppler beaming effect, induced by the reflex motion of stars, introduces
flux modulations and serves as an efficient method to photometrically determine
mass functions for a large number of close binary systems, particularly those
involving compact objects. In order to convert observed beaming-flux variations
into a radial-velocity curve, precise determination of the beaming factor is
essential. Previously, this factor was calculated as a constant, assuming a
power-law profile for stellar spectra. In this study, we present a novel
approach to directly compute this factor. Our new method not only simplifies
the computation, especially for blue bands and cool stars, but also enables us
to evaluate whether the relationship between beaming flux and radial velocity
can be accurately described as linear. We develop a python code and compute a
comprehensive beaming-factor table for commonly used filter systems covering
main-sequence, subgiant, and giant stars, as well as hot subdwarf and white
dwarf stars. Both the code and our table are archived and publicly available at
http://doi.org/10.5281/zenodo.13049419.
