Detecting Stars at the Galactic Centre via Synchrotron Emission
  Stars orbiting within 1$\arcsec$ of the supermassive black hole in the
Galactic Centre, Sgr A*, are notoriously difficult to detect due to obscuration
by gas and dust. We show that some stars orbiting this region may be detectable
via synchrotron emission. In such instances, a bow shock forms around the star
and accelerates the electrons. We calculate that around the 10 GHz band (radio)
and at 10$^{14}$ Hz (infrared) the luminosity of a star orbiting the black hole
is comparable to the luminosity of Sgr A*. The strength of the synchrotron
emission depends on a number of factors including the star's orbital velocity.
Thus, the ideal time to observe the synchrotron flux is when the star is at
pericenter. The star S2 will be $\sim 0.015\arcsec$ from Sgr A* in 2018, and is
an excellent target to test our predictions.
