  The dynamics of the partially ionized solar atmosphere is controlled by the
frequent collision and charge exchange between the predominant neutral Hydrogen
atoms and charged ions. At signal frequencies below or of the order of either
of the collision or charge exchange frequencies the magnetic stress is {\it
felt} by both the charged and neutral particles simultaneously. The resulting
neutral-mass loading of the ions leads to the rescaling of the effective
ion-cyclotron frequency-it becomes the Hall frequency, and the resultant
effective Larmor radius becomes of the order of few kms. Thus the finite Larmor
radius (FLR) effect which manifests as the ion and neutral pressure stress
tensors operates over macroscopic scales. Whereas parallel and perpendicular
(with respect to the magnetic field) viscous momentum transport competes with
the Ohm and Hall diffusion of the magnetic field in the
photosphere-chromosphre, the gyroviscous effect becomes important only in the
transition region between the chromosphere and corona, where it competes with
the ambipolar diffusion. The wave propagation in the gyroviscous effect
dominated medium depends on the plasma $\beta$ (a ratio of the thermal and
magnetic energies). The abundance of free energy makes gyro waves unstable with
the onset condition exactly opposite of the Hall instability. However, the
maximum growth rate is identical to the Hall instability. For a flow gradient
$\sim 0.1 \,\mbox{s}^{-1}$ the instability growth time is one minute. Thus, the
transition region may become subject to this fast growing, gyroviscous
instability.
