M-type stars are the most numerous stars in the universe. They are ideal host for the search of exoplanets in the habitable zone, as their small size and low temperature make the HZ much closer in than solar twins. As fully convective low mass stars, they usually also exhibit very intense magnetic fields. Understanding their environment, in particular their coronal and wind properties, is thus very important, as they might be very different from what is observed for the solar system. The mass loss rate of M-type stars is poorly known observationally, and recent attempts to estimate some of them (TRAPPIST, Proxima Cen) can vary by one order of magnitude. In this talk, I will take advantage of an Alfvén wave turbulence wind model, tested on many solar wind observables, to investigate the range of mass loss of a typical M-type star like TRAPPIST. I will show that chromospehric and coronal radiative losses likely play a critical role in determining the energy budget of the stellar wind. I will also constrain the amplitude of the turbulent forcing amplitude using the X-ray/mass loss law of Wood et al., and compare it with convective properties of M-dwarf.