  We discuss the properties of pulsations in the OGLE Small Amplitude Red
Giants (OSARGs) in the Large Magellanic Cloud (LMC). We consider stars below
the red-giant tip in this paper. They are multi-periodic and form three
sequences in the period-luminosity plane. Comparing the periods and period
ratios with our theoretical models, we have found that these sequences
correspond to radial first to third overtones, and nonradial dipole p$_4$ and
quadrupole p$_2$ modes. The red-giant branch stars of OSARGs consist of stars
have initial masses of $\sim0.9 - 1.4M_\odot$ which corresponds to a luminosity
range of $\log L/L_\odot \simeq 2.8 - 3.4$. With these parameters, the scaled
optimal frequency $\nu_{\rm max}$ for solar-like oscillations goes through
roughly the middle of the three sequences in the period-luminosity plane,
suggesting the stochastic excitation is likely the cause of the pulsations in
OSARGs.
