  We present new HI observations of the nearby massive spiral galaxy M83, taken
with the VLA at $21^{\prime\prime}$ angular resolution ($\approx500$ pc) of an
extended ($\sim$1.5 deg$^2$) 10-point mosaic combined with GBT single dish
data. We study the super-extended HI disk of M83 (${\sim}$50 kpc in radius), in
particular disc kinematics, rotation and the turbulent nature of the atomic
interstellar medium. We define distinct regions in the outer disk ($r_{\rm
gal}>$central optical disk), including ring, southern area, and southern and
northern arm. We examine HI gas surface density, velocity dispersion and
non-circular motions in the outskirts, which we compare to the inner optical
disk. We find an increase of velocity dispersion ($\sigma_v$) towards the
pronounced HI ring, indicative of more turbulent HI gas. Additionally, we
report over a large galactocentric radius range (until $r_{\rm gal}{\sim}$50
kpc) that $\sigma_v$ is slightly larger than thermal (i.e. $>8$km s$^{-1}$ ).
We find that a higher star formation rate (as traced by FUV emission) is not
always necessarily associated with a higher HI velocity dispersion, suggesting
that radial transport could be a dominant driver for the enhanced velocity
dispersion. We further find a possible branch that connects the extended HI
disk to the dwarf irregular galaxy UGCA365, that deviates from the general
direction of the northern arm. Lastly, we compare mass flow rate profiles
(based on 2D and 3D tilted ring models) and find evidence for outflowing gas at
r$_{\rm gal}$ $\sim$2 kpc, inflowing gas at r$_{\rm gal}$ $\sim$5.5 kpc and
outflowing gas at r$_{\rm gal}$ $\sim$14 kpc. We caution that mass flow rates
are highly sensitive to the assumed kinematic disk parameters, in particular,
to the inclination.
