DYNAMICAL EVIDENCE FOR A MAGNETOCENTRIFUGAL WIND FROM A 20 M{sub Sun} BINARY YOUNG STELLAR OBJECT
Journal Article
·
· Astrophysical Journal Letters
- Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States)
- Joint Institute for VLBI in Europe, Postbus 2 7990 AA, Dwingeloo (Netherlands)
- NRAO, P.O. Box O, Socorro, NM 87801 (United States)
In Orion BN/KL, proper motions of {lambda}7 mm vibrationally excited SiO masers trace the rotation of a nearly edge-on disk and a bipolar wide-angle outflow 10-100 AU from radio source I, a binary young stellar object of {approx}20 M{sub Sun }. Here we map ground-state {lambda}7 mm SiO emission with the Very Large Array and track proper motions over 9 yr. The innermost and strongest emission lies in two extended arcs bracketing Source I. The proper motions trace a northeast-southwest bipolar outflow 100-1000 AU from Source I with a median three-dimensional motion of {approx}18 km s{sup -1}. An overlying distribution of {lambda}1.3 cm H{sub 2}O masers betrays similar flow characteristics. Gas dynamics and emission morphology traced by the masers suggest the presence of a magnetocentrifugal disk wind. Reinforcing evidence lies in the colinearity of the flow, apparent rotation across the flow parallel to the disk rotation, and recollimation that narrows the flow opening angle {approx}120 AU downstream. The arcs of ground-state SiO emission may mark the transition point to a shocked super-Alfvenic outflow.
- OSTI ID:
- 22118703
- Journal Information:
- Astrophysical Journal Letters, Journal Name: Astrophysical Journal Letters Journal Issue: 2 Vol. 770; ISSN 2041-8205
- Country of Publication:
- United States
- Language:
- English
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