Abstract
The discovery of the first brown dwarfs (Rebolo et al. 1995, Nakajima et al. 1995) has posed an important problem to theoretical and observational astronomers: the formation mechanism. Reipurth & Clark (2001) have proposed that they form as stellar embryos, which gravitationally interact in multiple systems, are rapidly expelled and, therefore, are unable to accrete enough matter to become low mass stars. On the contrary, Padoan & Norlund (2002) argue that they are formed by collapse and fragmentation of a cloud (i.e., as stars do). These scenarios can be tested from the observational point of view, since kinematics, the statistics of circum(sub)stellar disks and their properties should be different. Then, the firs step is to identify such disks and study their properties. In other words, if brown dwarfs experience a phase similar to Classical Tstars, this fact would be a strong evidence that the formation mechanism is similar.
