Spectroscopic diagnosis of warm MHD winds

Self-similar models for warm MHD disk winds have been analyzed following Sakurai (1985) and Vlahakis et al (2000) formulations. The winds are assumed to depart from keplerian rings of warm gas (T = 10 K) which could be formed in the corona of accretion disk or in the stellar magnetosphere-inner accretion disk interaction region where magnetic energy is dissipated and heats the gas. The models provide a detailed solution for the bipolar flow, e.g., thermal, density and velocity laws, which has been used to determine the emissivity of the most relevant forbidden lines. The ultraviolet semiforbidden lines of CIII](190.8nm) and SiIII](189.2nm) are shown to be good tracers of the inner (and unresolved) wind region. The main signature of the winds is generating broad wings, with FWHM around few 100 km/s on the profiles of these lines which adds to the stellar atmosphere contribution.