  Fuzzy Dark Matter (FDM), consisting of ultralight bosons, is an intriguing
alternative to Cold Dark Matter. Numerical simulations solving the
Schr\"odinger-Poisson (SP) equation, which governs FDM dynamics, show that FDM
halos consist of a central solitonic core (representing the ground state of the
SP equation), surrounded by a large envelope of excited states. Wave
interference gives rise to order unity density fluctuations throughout the
envelope and causes the soliton to undergo density oscillations and execute a
confined random walk in the central region of the halo. The resulting
gravitational potential perturbations are an efficient source of dynamical
heating. Using high-resolution numerical simulations of a $6.6 \times 10^{9}
\rm M_{\odot}$ FDM halo with boson mass, $m_{\rm b}=8 \times 10^{-23} \ \rm
eV$, we investigate the impact of this dynamical heating on the structure and
kinematics of spheroidal dwarf galaxies of a fixed mass but different initial
sizes and ellipticities. The galaxies are set up in equilibrium in the
time-and-azimuthally averaged halo potential and evolved for $10 \ \rm Gyr$ in
the live FDM halo. We find that they continuously increase their sizes and
central velocity dispersions. In addition, their kinematic structures become
strongly radially anisotropic, especially in the outskirts. Dynamical heating
also causes initially ellipsoidal galaxies to become more spherical over time
from the inside out and gives rise to distorted, non-concentric isodensity
contours. These tell-tale characteristics of dynamical heating of dwarf
galaxies in FDM halos can potentially be used to constrain the boson mass.
