The short-term (27-day sequences) and long-term variabilities of solar line emissions (120--280 nm) and radio emissions (245--2800 MHz) were studied during 1991--2000. The amplitudes of the 27-day oscillations were obtained by Maximum Entropy Method (MEM) and Multiple Regression Analysis (MRA). The amplitudes were small (1--2%) near the solar surface and in the lower chromosphere, increased to ~10% in the upper chromosphere and lower transition region, decreased in the upper transition region, increased to ~12% in the lower corona, and decreased thereafter in the middle and upper corona. The long-term variability also showed qualitatively a similar pattern. The pattern is similar to the dip around 100,000 K observed in the emission measure distribution in the solar atmosphere.