We consider local , stratified , numerical models of isothermal accretion disks .
The novel feature of our treatment is that radial extent L _ { x } and azimuthal extent L _ { y } satisfy H \ll L _ { x } ,L _ { y } \ll R , where H is the scale height and R is the local radius .
This enables us to probe mesoscale structure in stratified thin disks .
We evolve the model at several resolutions , sizes , and initial magnetic field strengths .
Consistent with earlier work , we find that the saturated , turbulent state consists of a weakly magnetized disk midplane coupled to a strongly magnetized corona , with a transition at |z| \sim 2 H .
The saturated \alpha \simeq 0.01 - 0.02 .
A two-point correlation function analysis reveals that the central 4 H of the disk is dominated by small scale turbulence that is statistically similar to unstratified disk models , while the coronal magnetic fields are correlated on scales \sim 10 H .
Nevertheless angular momentum transport through the corona is small .
A study of magnetic field loops in the corona reveals few open field lines and predominantly toroidal loops with a characteristic distance between footpoints that is \sim H .
Finally we find quasi-periodic oscillations with characteristic timescale \sim 30 \Omega ^ { -1 } in the magnetic field energy density .
These oscillations are correlated with oscillations in the mean azimuthal field ; we present a phenomenological , alpha-dynamo model that captures most aspects of the oscillations .