Long-term homogeneous photometry for 35 classical T Tauri stars(CTTS)in the Taurus-Auriga star-forming region has been analyzed. Reliable interstellar extinctions, luminosities, effective temperatures, masses, ages, and radii have been determined for the CTTS. The physical parameters and evolutionary status of 34 weakline T Tauri stars(WTTS)from previous studies and 35 CTTS from this work have been compared. The rotation periods, radii, and luminosities of low-mass(0.3-1.1 M_⊙)CTTS are shown to be, on average, greater than those of low-mass WTTS, in good agreement with the evolutionary status of these two subgroups. The mean age of the younger subgroup of WTTS from our sample(2.3 Myr)essentially coincides with the mean duration of the protoplanetary disk accretion phase(2.3 Myr)for a representative sample of low-mass stars in seven young stellar clusters. The accretion disk dissipation time scale for the younger subgroup of CTTS(<4 Myr)in the Taurus-Auriga starforming region is shown to be no greater than 0.4 Myr, in good agreement with the short protoplanetary disk dissipation time scale that is predicted by present-day protoplanetary disk evolution models.
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