A detailed analysis of the ULF noise observed on the GEOS magnetic antennas in the frequency range ~0.2--12 Hz has revealed the properties of structured emissions occurring just above the proton gyrofrequency whose existence was reported by Russell et al. (1970) and Gurnett (1976). These waves are observed in the vicinity of the geomagnetic equator at all L values between ~4 and ~8. They propagate in a direction perpendicular to the dc magnetic field. The waves consist of harmonically related monochromatic emissions. The fundamental frequency is generally of the order of the local proton gyrofrequency. Sometimes the fundamental and first harmonics are missing. If there is more than one fundamental frequency present, nonlinear coupling often occurs between the different emissions. The amplitudes of individual events vary from some tens of milligammas to some hundreds. Their duration ranges from some tens of minutes to some hours. Within the range of sentitivity of the detectors (10-2&ggr; Hz-1/2 at 1 Hz, 10-3&ggr; Hz-1/2 at 8 Hz) the average probability of emission occurrence during a given hour is 12%, this number increases to ~30% during the afternoon and in the premidnight sectors. Simultaneous observations of proton fluxes, as obtained from the two GEOS particle experiments show that these waves are often associated with distribution functions peaking at some energy (5≲E≲30 keV) for 90¿ pitch angle particles. This ring-like distribution provides the energy source for the excitation of non resonant (k∥=0) instabilities near nFH+(n=running number). A theoretical model is presented that qualitatively explains the main characteristics of the observed waves.