BIMA Interferometer observations of dust continuum emission at 1.3 mm probe protostellar disk and envelope structures of the two brightest millimeter sources near SVS 13, from 0 .3 to 20 . The SVS 13 ridge is the site of a small group of deeply embedded protostars in NGC 1333 that are thought to be forming solar-type stars. Powerful molecular outflows suggest these sources are still engaged in the mass accretion process and may have substantial regions surrounding the central sources undergoing infall. High-resolution 1.3 mm data in conjunction with a previously published single-dish map at 1.3 mm (R. Chini et al. 1997, AA S. Terebey, F. H. Shu, & P. Cassen 1984, ApJ, 286, 529) that defines the division between collapse and quasi-static regions in the envelope. Using a measured line width to trace the sound speed in combination with the inferred collapse radius verifies that these systems are very young, only ≈ yr old. 4 2.9 # 10 Growth of dust grains to ≈1 cm in these young protostellar disks is detected using millimeter-wave spectral index comparisons of the dust emission in the protostellar envelope and disk. These are the first observations to have high resolution and sensitivity to large-scale structures and to sample the disks and envelopes in the same system at 110 and 220 GHz (110 GHz observations from L. W. Looney, L. G. Mundy, & W. J. Welch 2000, ApJ, 529, 477). The observations demonstrate the dust-mass opacity spectral index for the compact strucb ≈ 0 tures (disks) around SVS 13A and B, whereas for the largescale envelopes, (defined by and , after b 2 b b ≈ 2 F ∝ n k ∝ n n n