Doppler Boosting of the S-stars in the Galactic Center
  Astrometry and spectroscopy of the S-stars in the Galactic Center provide a
unique way to probe the properties of the central supermassive black hole, as
well as the post-Newtonian effects caused by its gravity, e.g. gravitational
redshift and general relativistic precession. It has also been suggested that
the photometry of S-stars can be used for studying the properties of gaseous
environment of Sgr A$^*$. Due to the high velocities of the S-stars, sometimes
approaching $~0.1c$, their photometric signal should be considerably affected
by the Doppler boosting. We calculate this relativistic effect for several
S-stars closely approaching the central black hole (most of them recently
announced) and show that the amplitude of the photometric variability due to
the Doppler boosting for some of them (S62 and S4714) exceeds $6\%$; for the
well studied star S2 it is about $2\%$. Measurement of the Doppler boosting can
confirm the existence and help refine orbital parameters of the S-stars with
noisy spectroscopy and astrometry. This effect should be explicitly accounted
for when the photometry of S-stars is used for probing the medium around the
Sgr A$^*$. We discuss the observability of the Doppler boosting given the
complications typical for the Galactic Center and conclude, in particular, that
the purely photometric detection of the higher order relativistic corrections
to the Doppler boosting signal (due to the gravitational redshift and
transverse Doppler shift, which we also calculate) is hardly possible for the
S-stars.
