  In addition to a supermassive black hole (SMBH), the central parsec of the
Milky Way hosts over a hundred of massive, high velocity young stars whose
existence, and organisation of a subset of them in one, or possibly two,
mis-aligned disks, is puzzling. Due to a combination of low medium density and
strong tidal forces in the vicinity of Sgr A*, stars are not expected to form.
Here we propose a novel scenario for their in-situ formation: a jetted tidal
disruption event (TDE) from an older wandering star triggers an episode of
positive feedback of star formation in the plane perpendicular to the jet, as
demonstrated via numerical simulations in the context of jet-induced feedback
in galactic outflows. An over-pressured cocoon surrounding the jet
shock-compresses clumps to densities high enough to resist the SMBH tidal
field. The TDE rate of $10^{-5}-10^{-4}$ yr$^{-1}$ per galaxy, out of which a
few percent events are jetted, implies a jetted TDE event per galaxy to occur
every few million years. This timescale is interestingly of the same order of
the age of the disk stars. The mass function predicted by our mechanism is
top-heavy. Additionally, since TDEs are isotropic, our model predicts a random
orientation for the disk of stars with respect to the plane of the galaxy and,
due to the relatively high TDE rate, it can account for multiple disks of stars
with uncorrelated orientations.
