  Low-mass stars appear to frequently host planetary systems. When these rocky
planets develop high eccentricities as a result of secular torques or dynamical
scatterings, they occasionally pass close to the host star. In these close
passages, planets can be tidally disrupted, and sheared into bound and unbound
debris tails. To suffer such a disruption the stellar density must by higher
than the planetary density. This condition is met for the most common star and
planet systems, M-dwarf stars hosting rocky planets. We describe the dynamics
of a tidal disruption, and estimate the typical velocities of unbound ejecta.
We simulate the gas dynamics of a planetary tidal disruption, and show that
disruptions preserve the layered structure of a rocky body, with the outermost
layers flung into interstellar space with the highest velocities. We compare
these properties to that of the candidate interstellar meteoroid
CNEOS-2014-01-08 (IM1). IM1's approximately 60~km~s$^{-1}$ excess speed
relative to the local standard of rest is naturally reproduced by the unbound
debris of the disruption of an Earth-like planet around an M-dwarf star. We
suggest that such an encounter might explain the interstellar kinematics of
IM1, and its unusual composition, especially if it originated in the
fastest-expelled crust of a differentiated rocky planet. Finally, we estimate
that the disruption of $\sim 10M_\oplus$ reservoirs of rocky planets per
M-dwarf are needed to reproduce the inferred rate of IM1-like objects.
