We are carrying out a study on the stellar content (age and metallicity) along the bars in a small sample of barred spirals of different morphological types (SB0~SBb). The goal is to search for observational evidence of the evolution of stellar populations in barred spirals, and to compare with the predictions of numerical models found in the literature for the evolution of bars (e.g. Friedli and Benz: 1995, A&A 301, 649). We measure a large set of spectral indices (mainly the Lick system of indices, plus the CaII NIR triplet), complemented with optical-NIR color maps. Comparing them with stellar population synthesis models, we try to determine the mean luminosity-weighted age and metallicity of the (spatially averaged) stellar populations along the bars. We focus on the relative ages/metallicities, as absolute values are quite uncertain and more model dependent.We have found evidence of a difference in the mean stellar age between the nuclear and circumnuclear ring (CNR) of the SBa galaxy NGC 4314, greater than (at least) 3–4 Gyr. Also, there is a hint that a relatively small amount of gas has been supplied to the nuclear region by the bar, as shown by the spectra, broad-band images and line strength diagrams. We have found Mg overabundant relative to Fe in the nuclear region. Some of the uncertainties in the comparison of model predictions and observations are investigated (Lourenso et al.: 2001b, Ap&SS, in press). Recent results show a tight linear distribution in the color-magnitude and color-color diagrams along the nuclear spiral arms of NGC 4314, getting redder and fainter from the CNR outwards and suggesting, in principle, an age sequence (Lourenso et al.: 2001c, in prep.). A discussion on the stellar populations of the prototype double-barred galaxy NGC 5850 (SBb) will be presented in Lourenso et al. (200la, ApJ, submitted).