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Low spatial resolution observations in the range 3900A to 9000A of solar active regions have been compared to similar observations of the active components of three RS CVn binaries. The solar observations were obtained in 1989 with a solar echelle spectrograph and CCD (charge-coupled device) camera on the 6-inch guide telescope at Penn State's Black Moshannon Observatory. The stellar observations were obtained in 1987 and 1988 with the FOE (fiber optic echelle) spectrograph and CCD on the coude feed at Kitt Peak National Observatory. Excess emission profiles of H$\\alpha$, H$\\beta$, and the 8498A and 8542A lines of the Ca II infrared triplet have been analyzed. The ratio of the energy emitted in H$\\alpha$ to H$\\beta$ is much smaller in solar plages than in RS CVn active subgiants. The character of the infrared triplet emission is also different. Analysis of these differences and the phase behavior of the Balmer and infrared triplet lines in the RS CVns suggests that the Balmer emission originates from different emitting structures than the infrared triplet. In agreement with Buzasi (1989), the Balmer emission is produced primarily in prominence-like extended material. The Ca II infrared triplet emission appears to be largely plage-related. Emission in the far wings of the Balmer lines may also arise in plages.