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(Abridged) We analyze the evolution of 42 spiral galaxies in the SpitzerInfrared Nearby Galaxies Survey, using extinction-corrected UV, optical andnear-infrared radial profiles to probe the emission of stars of different agesas a function of radius. We fit these profiles with models that describe thechemical and spectro-photometric evolution of spiral disks within aself-consistent framework. These backward models succesfully reproduce themulti-wavelength profiles of our galaxies, except the UV profiles of someearly-type disks. From the model fitting we infer the maximum circular velocityof the rotation curve (Vc) and the dimensionless spin parameter (lambda). Thevalues of Vc are in good agreement with the velocities measured in HI rotationcurves. While our sample is not volume-limited, the resulting distribution ofspins is close to the lognormal function obtained in cosmological N-bodysimulations, peaking at ~0.03 regardless of the total halo mass. We do not findany evident trend between spin and Hubble type, besides an increase in thescatter for the latest types. According to the model, galaxies evolve along aroughly constant mass-size relation, increasing their scale-lengths as theybecome more massive. The radial scale-length of most disks in our sample seemsto have increased at a rate of 0.05-0.06 kpc/Gyr, being now 20-25% larger thanat z=1.

Radial distribution of stars, gas and dust in SINGS galaxies. III. Modeling the evolution of the stellar component in galaxy disks