Despite theoretical predictions on the existence of solar gravity oscillations (g modes), their detection is still marginal. The main reasons are their frequencies, ν<0.2 mHz, and amplitudes of
less than 10 cm/s. However, because these modes are extremely sensitive to the physical conditions in the very deep sun, they can give us detailed Information on the physics of the core. Using a resontant scattering spectrophotometer we measured the radial velocity of the Sun at the KI 769.9 nm. line with very high resolution and temporal stability. The observatíons carried out at Izaňa (Tenerife) continuously for the last three years, háve been used to search for solar g modes. Analysis of the whole lot of data as one single time series provides a spectral resolution of 12 nHz, and signal with amplitude above noise level, 1 cm/s. Several techniques are used in order to find.the signature of g modes and calculate the parameters Po and vr. Individua! peaks, well above noise level, are identified and their frequencies are likely to correspond with
g modes.