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We investigate the possibility to apply the already suggested by Sarafopoulos(2017, 2019) main concept of dynamo action to red dwarfs and red giant andsupergiant stars. Thus, we attempt to establish a unified dynamo action, beingpotentially at work at widely varying stellar domains. Thus, the powerful,unique and leading entity generating the primary stellar magnetic field remainsthe so-called Torus structure. Within the Torus the same sign charges aremutually attracted and the Torus could be simulated as a superconductor. Anexisting gradient of the rotation rate accumulates net charge in the Torus, andthe resulting toroidal current becomes the driving source of the magneticfield. In turn, there is a complicated network of secondary interactions thataffect and modulate the whole star's magnetic behaviour. Our dynamo action ispotentially at work in fully and partly convecting stars. A major finding isthat 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 largerthe star, the deeper inward the Torus is formed. The formation of a singleTorus is essentially associated with a large-scale strong, poloidal andaxisymmetric magnetic field topology, whereas the generation of a weakermultipolar, non-axisymmetric field configuration in rapid evolution can resultfrom a double-Torus structure (like the solar case). The same basic concept isscaled up or down. Moreover, we identify four key parameters associated withthe magnetic field of red dwarfs, giants and supergiants: First, the rotationspeed; second, the steepness of the radial gradient of the rotation rate in theshear 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 areintroduced for the first time.

The dynamo action for red dwarfs and red giant and supergiant stars