Abstract Due to the relatively large cosmic abundance of Si and the stability of colored silicon compounds easily formed under various nonequilibrium conditions, it is concluded here that silicon should be strongly considered as a potential major component in the observed colored material in the Jupiter atmosphere. Silicon is one of the most abundant elements in the universe (after H, He, 0, N, and C) and in the same order of abundance as Mg and Fe. In the high temperature and pressure regions of Jupiter most of the Si should be present as SiH4. At higher altitudes, corresponding to a total pressure of less than 1000 bar and a temperature below 1200 K, SiC>2 and other compounds of silicon should dominate. These equilibria and the chemistry depend strongly upon the H9O concentration, which is assumed to be in the order of 10~ 3 . A calculated equilibrium profile had been proposed for a model atmosphere [1] and our own estimates confirm the main features within reasonable limits. Recent photographs taken of Jupiter emphasize the fact that the atmosphere of the planet is not in equilibrium. Atmospheric turbulence is observed corresponding to movement in the colored areas including the well-known great red spot. Assuming, therefore, that non-equilibrium processes may occur on Jupiter, the nature of such processes may be sought in the laboratory. The non-equilibrium transition of SiH4 to Si(>2 can be observed in various ways. We have found that many of these lead to intermediates that are relatively stable and yield strong colorations very similar in appearance to those observed on Jupiter. The purpose of this paper is to emphasize the possibility of the silicon compounds contributing