Solar-like oscillations in late spectral class stars

We investigate the minimum mass star that can exhibit solar-like nonradial p-mode oscillations. Solar models have almost equal pulsational driving and damping due to standard radiative effects. Coupling with surface convective elements occasionally tips the balance by strongly driving for a few days modes with convection timescales at the top of the convection zone. Then both convective and radiative damping decrease the mode amplitude at an observed decay rate until the next convective reexcitation. Population I stellar models at 0.30, 0.45 and 0.75 solar mass have been constructed to see if they have a near equality of radiative driving and damping also. If so, then stars down to late spectral class could possibly display solar-like oscillations. We find that the near equality of radiative driving and damping occurs down to about 0.5 solar mass. Possibly 100 to 300 second oscillations can be observed through most of the K spectral class, if magnetic activity does not overwhelm these small amplitude nonradial pulsations