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Recently, surface magnetic field maps had been acquired for a small sample ofactive M dwarfs, showing that fully convective stars (spectral types ~M4 andlater) host intense (~kG), mainly axi-symmetrical poloidal fields. Inparticular, the rapidly rotating M dwarf V374Peg (M4), believed to lie near thetheoretical full convection threshold, presents a stable magnetic topology on atime-scale of 1 yr. The rapid rotation of V374Peg (P=0.44 days) along with itsintense magnetic field point toward a magneto-centrifugally acceleration of acoronal wind. In this work, we aim at investigating the structure of thecoronal magnetic field in the M dwarf V374Peg by means of three-dimensionalmagnetohydrodynamical (MHD) numerical simulations of the coronal wind. For thefirst time, an observationally derived surface magnetic field map isimplemented in MHD models of stellar winds for a low-mass star. Weself-consistently take into consideration the interaction of the outflowingwind with the magnetic field and vice versa. Hence, from the interplay betweenmagnetic forces and wind forces, we are able to determine the configuration ofthe magnetic field and the structure of the coronal winds. Our results enableus to evaluate the angular momentum loss of the rapidly rotating M dwarfV374Peg.

Understanding the Angular Momentum Loss of Low-Mass Stars: The Case of V374 Peg