As the observations of highly flattened galaxies including the Milky Way and many-body (N-body) simulations show, the central parts of these systems, say, at distances r < 0.5–0.7 kpc from the center, rotate slowly and their local circular velocities of regular rotation become less than (or comparable to) the residual (random) velocities. In such a thin, practically nonrotating circumnuclear disk, a typical star moves along the bending, perpendicular to the equatorial plane layer under the action of two forces which act in opposite directions: the destabilizing centrifugal force Fc and the restoring gravitational attraction Fg. Obviously, fierce instabilities of the buckling kind developing perpendicular to the plane may not be avoided if Fc > Fg. The latter condition is none other than the condition of “firehose” electromagnetic instability in collisionless plasmas which is driven by the particle “pressure” anisotropy.