  T Tauri stars are young, low mass, pre-main sequence stars surrounded by an
accretion disk. These objects present strong magnetic activity and powerful
magnetic reconnection events. Strong shocks are likely associated with fast
reconnection in the stellar magnetosphere. Such shocks can accelerate particles
up to relativistic energies. We aim at developing a simple model to calculate
the radiation produced by non-thermal relativistic particles in the environment
of T Tauri stars. We want to establish whether this emission is detectable at
high energies with the available or forthcoming gamma-ray telescopes. We assume
that particles (protons and electrons) pre-accelerated in reconnection events
are accelerated at shocks through Fermi mechanism and we study the high-energy
emission produced by the dominant radiative processes. We calculate the
spectral energy distribution of T Tauri stars up to high-energies and we
compare the integrated flux obtained with that from a specific Fermi source,
1FGL J1625.8-2429c, that we tentatively associate with this kind of young
stellar objects (YSOs). We suggest that under reasonable general conditions
nearby T Tauri stars might be detected at high energies and be responsible for
some unidentified Fermi sources on the Galactic plane.
