We present new results from the DisksatEVLA program for two young stars: CY Tau and DoAr 25. We trace continuum emission arising from their circusmtellar disks from spatially resolved observations, down to tens of AU scales, at lambda = 0.9, 2.8, 8.0, 9.8 mm for DoAr 25 and at lambda = 1.3, 2.8, 7.1 mm for CY Tau. Additionally, we constrain the amount of emission whose origin is different from thermal dust emission from 5 cm observations. Directly from interferometric data, we find that observations at 7 mm and 1 cm trace emission from a compact disk while millimeter-wave observations trace an extended disk structure. From a physical disk model, where we characterize the disk structure of CY Tau and DoAr 25 at wavelengths shorter than 5 cm, we find that (1) dust continuum emission is optically thin at the observed wavelengths and over the spatial scales studied, (2) a constant value of the dust opacity is not warranted by our observations, and (3) a high-significance radial gradient of the dust opacity spectral index, beta , is consistent with the observed dust emission in both disks, with low- beta in the inner disk and high- beta in the outer disk. Assuming that changes in dust properties arise solely due to changes in the maximum particle size ( alpha sub(max)), we constrain radial variations of alpha sub(max) in both disks, from cm-sized particles in the inner disk (R < 40 AU) to millimeter sizes in the outer disk (R > 80 AU). These observational constraints agree with theoretical predictions of the radial-drift barrier, however, fragmentation of dust grains could explain our alpha sub(max)(R) constraints if these disks have lower turbulence and/or if dust can survive high-velocity collisions.