In accordance with the concepts of dynamo theory, largescale magnetic fields of many astrophysical objects are associated with the rotationinduced break of mirror symmetry (1). The rotation of objects and the presence of depth density gradients (∇ρ) turn out to be sufficient for the existence of a correlation between the vertical velocity and the vorticity of small� scale vortices. This correlation results in the nonzero kinetic helicity χ = 〈v · rotv〉, where v is the turbulent velocity and 〈·〉 implies averaging over an ensemble. In the simplest cases, it is considered that, in the same hemisphere, the helicity is of identical sign: in the northern hemisphere, it is negative when the density increases with depth, which is natural for selfgravitat� ing bodies. In the southern hemisphere, the helicity is positive, e.g., χ = -cosϑ (2, 3), where ϑ is the angle with respect to the rotation z axis in the spherical coor� dinate system (r, ϑ, ϕ). The existence of the nonzero helicity χ of the hemispheres significantly simplifies the generation of a largescale magnetic field. At the same time, the helicity is obtained as a result of aver� aging and is subjected to random fluctuations (4), which, in the long run, affects the generation of the magnetic field (5). The source of the fluctuations can be either an insufficient number of vortices over which averaging is performed or the existence of anomalies at the object boundaries, e.g., the appearance of tidal forces in binary stars or the presence of thermal inho� mogeneities at boundaries of the liquid core and the mantle in planets (6). These arguments can lead to the break of antisymmetry χ with respect to the equatorial plane. In the framework of the Parker model for the αω dynamo, we show below that, even for a linear mode, a small nonparity (χ) violation can lead to a sig� nificant symmetry break of the magnetic field in oppo� site hemispheres. We now consider the Parker model often applied to describe processes of the magneticfield generation in various astrophysical objects (1, 7, 8). We below make use of the following equations in a thin spherical shell: