Young stars are well known for being strong X-ray emitters. This emission can be originated by different processes: the active corona of the young star, by the accretion of matter from the disk into the star, or it can be originated in shocks. The high-energy photons affect the evolution of the disk of the pre-main sequence star and can have an influence in the planet formation process. In this thesis I studied the X-ray emission from pre-main sequence stars through high-resolution spectroscopy obtained with the Chandra Space Telescope, the goal was to characterize the coronal emission in such stars. The next step of my research was to study the effects of high-energy emission in the proto-planetary disks environments through spectroscopy in the mid-infrared and optical. I focused on gas emission lines in the mid-infrared, in particular the [Ne II] line at 12.8 microns. This line has been observed in many T Tauri disks with Spitzer and the origin of the emission is under debate. It has been claim to be a good tracer of stellar X-ray emission, but it can also be emitted by the photoevaporation of the disk and by jets