  Tidal disruption events with tidal radius $r_{\rm t}$ and pericenter distance
$r_{\rm p}$ are characterized by the quantity $\beta = r_{\rm t}/r_{\rm p}$,
and "deep encounters" have $\beta \gg 1$. It has been assumed that there is a
critical $\beta \equiv \beta_{\rm c} \sim 1$ that differentiates between
partial and full disruption: for $\beta < \beta_{\rm c}$ a fraction of the star
survives the tidal interaction with the black hole, while for $\beta >
\beta_{\rm c}$ the star is completely destroyed, and hence all deep encounters
should be full. Here we show that this assumption is incorrect by providing an
example of a $\beta = 16$ encounter between a $\gamma = 5/3$, solar-like
polytrope and a $10^6 M_{\odot}$ black hole -- for which previous
investigations have found $\beta_{\rm c} \simeq 0.9$ -- that results in the
reformation of a stellar core post-disruption that comprises approximately 25\%
of the original stellar mass. We propose that the core reforms under
self-gravity, which remains important because of the compression of the gas
both near pericenter, where the compression occurs out of the orbital plane,
and substantially after pericenter, where compression is within the plane. We
find that the core forms on a bound orbit about the black hole, and we discuss
the corresponding implications of our findings in the context of recently
observed, repeating nuclear transients.
