  Excitation of solar oscillations is attribued to turbulent motions in the
solar convective zone. It is also currently believed that oscillations of low
massive stars (M <2 Mo) - which possess an upper convective zone - are
stochastically excited by turbulent convection in their outer layers.
  A recent theoretical work (Samadi & Goupil, 2001 ; Samadi et al, 2001)
supplements and reinforces this theory. This allows the use of any available
model of turbulence and emphasizes some recent unsolved problems which are
brought up by these new theoretical developments.
