Abstract
We have constructed models of stars which form by accretion from a disk. We have calculated accretion and pre-main-sequence evolutionary tracks for a range of initial parameters which spans the physically reasonable modes for accretion. We find that these models agree with the observed positions of T Tauri stars in the H-R diagram and avoid some of the problems which were endemic to traditional pre-main-sequence evolution. We find no evidence to indiccate that the formation of high- and low-mass stars in young open clusters is noncoeval. We point out a problem that arises when one attempts to use an H-R diagram of T Tauri stars to distinguish between various models of star formation.
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