The Mass Evolution Of Envelopes & Disks During The Embedded Protostellar Stage

Details The Mass Evolution Of Envelopes & Disks During The Embedded Protostellar Stage The Mass Evolution Of Envelopes & Disks During The Embedded Protostellar Stage

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21734035b&link_type=abstract

American Astronomical Society, AAS Meeting #217, #340.35; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astronomy

Scientific paper

A key question in protostellar evolution is how is matter accreted from the large-scale envelope thought the circumstellar disk and onto the
central protostar. Observations that measure the mass of these components are needed to provide constraints on models of mass evolution and disk growth in the earlier (embedded) phase
of protostellar evolution. Previously we presented a study of a sample of 20 low-mass Class 0 and I protostars in Taurus and Ophuichus using the Submillimeter Array (SMA) and single-dish bolometer observations, with which the envelope and disk masses, and in some cases the protostellar mass, could be measured. We found that both Class 0 and I protostars are surrounded by disks with typical masses of about 0.05 solar masses, with large scatter, suggesting no correlation between disk mass and evolutionary stage. However, envelope masses decrease rather abruptly from 1 solar mass in the Class 0 phase to 0.1 solar mass in the Class I phase. Typically in the Class 0 phase envelopes contain 10 times or more mass than disks, but only 2-4 times the disk mass during the Class I phase. These results suggest that disks are formed early in protostellar evolution and that matter is accreted and dispersed rapidly from the envelope. Here we present the results of an expanded study, including a significant increase in the number of sources and regions observed with the SMA.
This work is supported by NASA Origins grant NXX09AB89G.

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