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In this paper, we study the quasinormal modes of the massless Dirac field forcharged black holes in Rastall gravity. The spherically symmetric black holesolutions in question are characterized by the presence of a power-Maxwellfield, surrounded by the quintessence fluid. The calculations are carried outby employing the WKB approximations up to the thirteenth order, as well as thematrix method. The temporal evolution of the quasinormal modes is investigatedby using the finite difference method. Through numerical simulations, theproperties of the quasinormal frequencies are analyzed, including those for theextremal black holes. Among others, we explore the case of a second type ofextremal black holes regarding the Nariai solution, where the cosmical andevent horizon coincide. The results obtained by the WKB approaches are found tobe mostly consistent with those by the matrix method. It is demonstrated thatthe black hole solutions for Rastall gravity in asymptotically flat spacetimesare equivalent to those in Einstein gravity, featured by different asymptoticalspacetime properties. As one of its possible consequences, we also investigatethe behavior of the late-time tails of quasinormal models in the present model.It is found that the asymptotical behavior of the late-time tails ofquasinormal modes in Rastall theory is governed by the asymptotical propertiesof the spacetimes of their counterparts in Einstein gravity.

Dirac quasinormal modes of power-Maxwell charged black holes in Rastall gravity