  The temperatures of observed protoplanetary disks are not sufficiently high
to produce the accretion rate needed to form stars, nor are they sufficient to
explain the volatile depletion patterns in CM, CO, and CV chondrites and
terrestrial planets. We revisit the role that stellar outbursts, caused by high
accretion episodes, play in resolving these two issues. These outbursts provide
the necessary mass to form the star during the disk lifetime, and provide
enough heat to vaporize planet-forming materials. We show that these outbursts
can reproduce the observed chondrite abundances at distances near one AU. These
outbursts would also affect the growth of calcium-aluminum-rich inclusions
(CAIs) and the isotopic compositions of carbonaceous and non-carbonaceous
chondrites.
