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In this work we investigate the characteristics of the group velocity ofobliquely propagating Alfv\'en waves in a dusty plasma typical of a stellarwind. The dispersion relation is derived with the aid of the kinetic theory fora magnetized dusty plasma consisting of electrons and ions, with distributionof momenta described by a Maxwellian function. The dust particles areconsidered to be immobile and have all the same size; they are electricallycharged by absorption of plasma particles via inelastic collisions and byphotoionization. We numerically solve the dispersion relation and calculate thecomponents of group velocity (along and transverse to the magnetic field) forthe normal modes, namely the compressional and shear Alfv\'en waves (CAW andSAW). The results show that the direction of the group velocity of CAWs isgreatly modified with the wave-vector direction. On the other hand, SAWs willpresent group velocity propagating practically along the magnetic field. Thechanges in dust parameters, such as number density and equilibrium electricalcharge, may significantly change the waves' characteristics. It is seen thatfor sufficiently high dust to ion number density ratio, the SAWs may presentperpendicular group velocity propagating in opposite direction to theperpendicular phase velocity, in a small interval of wavenumber values; we alsonotice that this interval may change, or even vanish, when the flux ofradiation incident on the dust is altered, changing the equilibrium electricalcharge of the grains.

Group velocity of obliquely propagating Alfv\'en waves in a magnetized dusty plasma