Recently , surface magnetic field maps had been acquired for a small sample of active M dwarfs , showing that fully convective stars ( spectral types \sim M4 and later ) host intense ( \sim kG ) , mainly axi-symmetrical poloidal fields .
In particular , the rapidly rotating M dwarf V374 Peg ( M4 ) , believed to lie near the theoretical full convection threshold , presents a stable magnetic topology on a time-scale of \sim 1 yr .
The rapid rotation of V374 Peg ( P = 0.44 days ) along with its intense magnetic field point toward a magneto-centrifugally acceleration of a coronal wind .
In this work , we aim at investigating the structure of the coronal magnetic field in the M dwarf V374 Peg by means of three-dimensional magnetohydrodynamical ( MHD ) numerical simulations of the coronal wind .
For the first time , an observationally derived surface magnetic field map is implemented in MHD models of stellar winds for a low-mass star .
We self-consistently take into consideration the interaction of the outflowing wind with the magnetic field and vice versa .
Hence , from the interplay between magnetic forces and wind forces , we are able to determine the configuration of the magnetic field and the structure of the coronal winds .
Our results enable us to evaluate the angular momentum loss of the rapidly rotating M dwarf V374 Peg .