  We compare the results of high-resolution simulations of individual dark
matter subhalos evolving in external tidal fields with and without baryonic
bulge and disk components, where the average dark matter particle mass is three
orders of magnitude smaller than cosmological zoom-in simulations of galaxy
formation. The Via Lactea II simulation is used to setup our initial conditions
and provides a basis for our simulations of subhalos in a dark matter-only
tidal field, while an observationally motivated model for the Milky Way is used
for the tidal field that is comprised of a dark matter halo, a stellar disk,
and a stellar bulge. Our simulations indicate that including stellar components
in the tidal field results in the number of subhalos in Milky Way-like galaxies
being only $65\%$ of what is predicted by $\Lambda$ Cold Dark Matter
($\Lambda$CDM). For subhalos with small pericentres $(r_p \lesssim 25$ kpc),
the subhalo abundance is reduced further to $40\%$, with the surviving subhalos
being less dense and having a tangentially-anisotropic orbital distribution.
Conversely, subhalos with larger pericentres are minimally affected by the
inclusion of a stellar component in the tidal field, with the total number of
outer subhalos $\approx 75\%$ of the $\Lambda$CDM prediction. The densities of
outer subhalos are comparable to predictions from $\Lambda$CDM, with the
subhalos having an isotropic distribution of orbits. These ratios are higher
than those found in previous studies that include the effects baryonic matter,
which are affected by spurious disruption caused by low resolution.
