Depletion of bright red giants in the Galactic center during its active
  phases
  Observations in the near-infrared domain showed the presence of the flat core
of bright late-type stars inside $\sim 0.5\,{\rm pc}$ from the Galactic center
supermassive black hole (Sgr A*), while young massive OB/Wolf-Rayet stars form
a cusp. Several dynamical processes were proposed to explain this apparent
paradox of the distribution of the Galactic center stellar populations. Given
the mounting evidence about a significantly increased activity of Sgr A* during
the past million years, we propose a scenario based on the interaction between
the late-type giants and a nuclear jet, whose past existence and energetics can
be inferred from the presence of $\gamma$-ray Fermi bubbles and bipolar radio
bubbles. Extended, loose envelopes of red giant stars can be ablated by the jet
with kinetic luminosity in the range of $L_{\rm j}\approx
10^{41}$-$10^{44}\,{\rm erg\,s^{-1}}$ within the inner $\sim 0.04\,{\rm pc}$ of
Sgr A* (S cluster region), which would lead to their infrared luminosity
decrease after several thousand jet-star interactions. The ablation of the
atmospheres of red giants is complemented by the process of tidal stripping
that operates at distances of $\lesssim 1\,{\rm mpc}$, and by the direct
mechanical interaction of stars with a clumpy disc at $\gtrsim 0.04\,{\rm pc}$,
which can explain the flat density profile of bright late-type stars inside the
inner half parsec from Sgr A*.
