  We investigate the possibility to apply the already suggested by Sarafopoulos
(2017, 2019) main concept of dynamo action to red dwarfs and red giant and
supergiant stars. Thus, we attempt to establish a unified dynamo action, being
potentially at work at widely varying stellar domains. Thus, the powerful,
unique and leading entity generating the primary stellar magnetic field remains
the so-called Torus structure. Within the Torus the same sign charges are
mutually attracted and the Torus could be simulated as a superconductor. An
existing gradient of the rotation rate accumulates net charge in the Torus, and
the resulting toroidal current becomes the driving source of the magnetic
field. In turn, there is a complicated network of secondary interactions that
affect and modulate the whole star's magnetic behaviour. Our dynamo action is
potentially at work in fully and partly convecting stars. A major finding is
that the strength of the magnetic field, for stars of the same spectral type,
is essentially controlled by the size of the star; we suggest that, the larger
the star, the deeper inward the Torus is formed. The formation of a single
Torus is essentially associated with a large-scale strong, poloidal and
axisymmetric magnetic field topology, whereas the generation of a weaker
multipolar, non-axisymmetric field configuration in rapid evolution can result
from a double-Torus structure (like the solar case). The same basic concept is
scaled up or down. Moreover, we identify four key parameters associated with
the magnetic field of red dwarfs, giants and supergiants: First, the rotation
speed; second, the steepness of the radial gradient of the rotation rate in the
shear layer; third, the distance of the Torus from the photosphere and fourth,
the cross-sectional area of the Torus. The third and fourth key parameters are
introduced for the first time.
