Infrared observations and general theoretical considerations lead to an inhomogeneous model of the Jovian atmospbere with two cloud layers: an upper semitransmitting cloud (assumed for to be negligibly thin) separated by a clear space from a lower cloud deck (assumed infinite). It is shown that the observed variation of the geometric albedo from the visible into the ultraviolet can be explained by the presence of fine absorbing particles in the atmosphere above the upper cloud deck. The apparent decrease of the geometric albedo from the visible into the infrared is shown to result mainly from molecular absorption bands, and it is argued that the continuum albedo remains high to at least 1 . An inhomogeneous model atmosphere calculated for T,,ff = 130 K is approximated by a set of homogeneous layers. Taking the upper cloud at a temperature of 140 K and the lower cloud top at 215 K, corresponding to abundances of 31 km-amagats and 108 km-amagats of H2 in the atmosphere, we find that the calculated equivalent widths of the H2 3-0 and 4-0 quadrupole bands are in good agreement with the observations for an upper cloud optical thickness of 3.5 and a particle conthrnum albedo of 0.99. With this atmospheric model, the calculated CH4 3v2-band equivalent widths are in agreement with the observations for an abundance ratio of CH4/H2 of about 8 X l0- , slightly higher than solar composition.