  Very low-mass stars and brown dwarfs can undergo pulsational instability
excited by central deuterium burning during the initial phases of their
evolution. We present the results of evolutionary and nonadiabatic linear
stability models that show the presence of unstable fundamental modes. The
pulsation periods vary bewteen ~5 hr for a 0.1 Msun star and ~1 hr for a 0.02
M$_\odot$ brown dwarf. The results are rather insensitive to variations in the
input physics of the models. We show the location of the instability strip in
the HR and c-m diagrams and discuss the observational searches for young
pulsators in nearby star forming regions.
