The Escape Velocity Curve of the Milky Way in Modified Newtonian
  Dynamics
  We determine the escape velocity from the Milky Way (MW) at a range of
Galactocentric radii in the context of Modified Newtonian Dynamics (MOND). Due
to its non-linear nature, escape is possible if the MW is considered embedded
in a constant external gravitational field (EF) from distant objects. We model
this situation using a fully self-consistent method based on a direct solution
of the governing equations out to several thousand disk scale lengths. We try
out a range of EF strengths and mass models for the MW in an attempt to match
the escape velocity measurements of Williams et al. (2017).
  A reasonable match is found if the EF on the MW is ${\sim 0.03 a_{_0}}$,
towards the higher end of the range considered. Our models include a hot gas
corona surrounding the MW, but our results suggest that this should have a very
low mass of ${\sim 2 \times 10^{10} M_\odot}$ to avoid pushing the escape
velocity too high. Our analysis favours a slightly lower baryonic disk mass
than the ${\sim 7 \times 10^{10} M_\odot}$ required to explain its rotation
curve in MOND. However, given the uncertainties, MOND is consistent with both
the locally measured amplitude of the MW rotation curve and its escape velocity
over Galactocentric distances of 8$-$50 kpc.
