[85.03] Mapping disks and outflow a few to 300 AU from two protostars in NGC2071

AAS 200th meeting, Albuquerque, NM, June 2002
Session 85. Stars: Disks, Shells and Variability
Oral, Thursday, June 6, 2002, 2:00-3:30pm, Ballroom A

[Previous] | [Session 85] | [Next]

[85.03] Mapping disks and outflow a few to 300 AU from two protostars in NGC2071

A. C. Seth (U. of Washington), L. J. Greenhill (CfA), B. P. Holder (U. of Texas)

NGC 2071IR is a region of intermediate mass star formation that hosts persistent water maser emission. We have mapped the emission associated with the infrared centers IRS1 and IRS3 at four epochs over five months with the Very Long Baseline Array, detecting 266 maser features with centrally peaked line profiles. We have detected proper motions for 29 features, corresponding to velocities of up to 38 km/sec. In both infrared centers, the water maser emission traces a disk and a collimated outflow component perpendicular to the disk. The disk components are both less than 20 AU in size. The outflows are larger, with flow speeds of ~25 km/sec extending up to 300 AU from the source. The IRS 1 outflow is complex, appearing to comprise of both a jet and expanding funnel-like cavity around the jet. The cavity walls may mark the interface between accreting and outflowing material. The IRS 1 disk shows proper motions that may provide direct detection of rotation in a protostellar disk.

The author(s) of this abstract have provided an email address for comments about the abstract: seth@astro.washington.edu

[Previous] | [Session 85] | [Next]