Since the installation of the Solar Submillimeter Telescope (SST) in 1999 in the Complejo Astronómico El Leoncito (CASLEO, Argentina), the almost unexplored solar emissions at frequencies >100 GHz started to reveal new insights about thermal and non-thermal processes in active regions. SST operates at the frequencies of 212 and 405 GHz providing the unique opportunity to distinguish and investigate emission mechanisms. We present a review of the most relevant findings obtained. An statistical study made with observations of a selected sample of active regions shows that their flux density spectra increase with frequency. Rapid brightenings (pulses) are always observed both at 212 and 405 GHz in association to solar flares lasting for some tens to hundreds of milliseconds. They are well correlated between the two frequencies and have flux spectra either flat or increasing with frequency. The flux of submillimeter wave pulses remain within the same order of magnitude for different bursts, ranging typically 100-300 s.f.u. at 212 GHz and 500-1000 s.f.u. at 405 GHz. The time evolution of the pulse occurrence rate usually reproduces the time profile of the X-rays/γ-rays emission, and the bulk emission at submillimeter waves, when the latter is observable. There are examples of good correlation between individual pulses at submillimeter waves and hard X-rays/γ-rays. Submillimeter pulses are not restricted to flare events, but appear to be a general phenomenon that occurs over active regions as well. The starting time of the rapid submillimeter wave pulses is coincident or precedes the projected launch time of the coronal mass ejections. SST observations of the November 4, 2003 large flare revealed a new and yet unknown spectral component with intensities increasing towards even higher frequencies, appearing along with, but separated from the well-known microwave component. © 2005 COSPAR. Published by Elsevier Ltd. 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