Several enigmatic dusty sources have been detected in the central parsec of
the Galactic Center. Among them is X7, located at only $\sim$0.02 pc from the
central super-massive black hole, Sagittarius A* (Sgr A*). Recent observations
have shown that it is becoming elongated due to the tidal forces of Sgr A*. X7
is expected to be fully disrupted during its pericenter passage around 2035
which might impact the accretion rate of Sgr A*. However, its origin and nature
are still unknown. We investigated the tidal interaction of X7 with Sgr A* in
order to constrain its origin. We tested the hypothesis that X7 was produced by
one of the observed stars with constrained dynamical properties in the vicinity
of Sgr A*. We employed a set of test-particle simulations to reproduce the
observed structure and dynamics of X7. The initial conditions of the models
were obtained by extrapolating the observationally constrained orbits of X7 and
the known stars into the past, making it possible to find the time and source
of origin by minimizing the three-dimensional separation and velocity
difference between them. Our results show that ejecta from the star S33/S0-30,
launched in $\sim$1950, can to a large extent, replicate the observed dynamics
and structure of X7, provided that it is initially elongated with a velocity
gradient across it, and with an initial maximum speed of $\sim$600~km~s$^{-1}$.
Our results show that a grazing collision between the star S33/S0-30 and a
field object such as a stellar mass black hole or a Jupiter-mass object is a
viable scenario to explain the origin of X7. Nevertheless, such encounters are
rare based on the observed stellar dynamics within the central parsec.

Este artículo explora los viajes en el tiempo y sus implicaciones.

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