  The evolution of a planet's atmosphere depends strongly on its host star's
properties. When their host stars are younger, planets can experience stronger
winds and EUV emissions. This is particularly true for planets orbiting
M-dwarfs due to their close proximity to the host star. To determine if these
planets retain an atmosphere, we consider the impacts from stellar wind and EUV
fluxes in driving atmospheric escape throughout the planet's lifetime. For
this, we determined the atmospheric mass loss due to stellar wind and
photoevaporation on 4 planets in close orbit and 34 in their star's habitable
zone (HZ). The M-dwarf host stars' wind velocity, density, and EUV flux were
calculated through rotation period and X-ray flux scaling over time. The mass
loss rate due to stellar wind and photoevaporation was then computed as a
function of time and accumulated throughout the planet's age to determine the
total atmospheric mass loss of the planet's initial H/He envelope. We find that
for HZ planets at orbits $<$ 0.1 AU, stellar wind can only remove $\leq 1\%$ of
the H/He envelope, while photoevaporation is essential for completely removing
the H/He envelope of most targets. Moreover, due to either mechanism, most
planets orbiting at $>$ 0.1 AU do not have their primordial envelope stripped.
Overall, out of the 38 planets studied, 13 were predicted to have lost the
primordial envelope due to photoevaporation, while 2 planets lost the envelope
due to both stellar wind and photoevaporation.
