Blowing Bubbles around Intermediate-Mass Stars: Feedback from
  Main-Sequence Winds is not Enough
  Numerous spherical ``shells" have been observed in young star-forming
environments that host low- and intermediate-mass stars. These observations
suggest that these shells may be produced by isotropic stellar wind feedback
from young main-sequence stars. However, the driving mechanism for these shells
remains uncertain because the momentum injected by winds is too low to explain
their sizes and dynamics due to their low mass-loss rates. However, these
studies neglect how the wind kinetic energy is transferred to the ISM and
instead assume it is instantly lost via radiation, suggesting that these shells
are momentum-driven. Intermediate-mass stars have fast ($v_w \gtrsim 1000$
km/s) stellar winds and therefore the energy injected by winds should produce
energy-driven adiabatic wind bubbles that are larger than momentum-driven wind
bubbles. Here, we explore if energy-driven wind feedback can produce the
observed shells by performing a series of 3D magneto-hydrodynamic simulations
of wind feedback from intermediate-mass and high-mass stars that are placed in
a magnetized, turbulent molecular cloud. We find that, for the high-mass stars
modeled, energy-driven wind feedback produces $\sim$pc scale wind bubbles in
molecular clouds that agree with the observed shell sizes but winds from
intermediate-mass stars can not produce similar shells because of their lower
mass-loss rates and velocities. Therefore, such shells must be driven by other
feedback processes inherent to low- and intermediate-mass star formation.
