THE MAGNETIC FIELD IN THE CLASS 0 PROTOSTELLAR DISK OF L1527
- Department of Astronomy, University of Illinois, Urbana, IL 61801 (United States)
- SRON Netherlands Institute for Space Research, Landleven 12, 9747 AD Groningen (Netherlands)
- National Radio Astronomy Observatory, Charlottesville, VA 22903 (United States)
- Astronomy Department, University of Virginia, Charlottesville, VA 22904 (United States)
We present subarcsecond (∼0.''35) resolved observations of the 1.3 mm dust polarization from the edge-on circumstellar disk around the Class 0 protostar L1527. The inferred magnetic field is consistent with a dominantly toroidal morphology; there is no significantly detected vertical poloidal component to which observations of an edge-on disk are most sensitive. This suggests that angular momentum transport in Class 0 protostars (when large amounts of material are fed down to the disk from the envelope and accreted onto the protostar) is driven mainly by magnetorotational instability rather than magnetocentrifugal winds at 50 AU scales. In addition, with the data to date there is an early, tentative trend that R > 30 AU disks have so far been found in Class 0 systems with average magnetic fields on the 1000 AU scale strongly misaligned with the rotation axis. The absence of such a disk in the aligned case could be due to efficient magnetic braking that disrupts disk formation. If this is the case, this implies that candidate Class 0 disk systems could be identified by the average magnetic field direction at ∼1000 AU spatial scales.
- OSTI ID:
- 22364779
- Journal Information:
- Astrophysical Journal Letters, Vol. 798, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 2041-8205
- Country of Publication:
- United States
- Language:
- English
Similar Records
On the role of pseudodisk warping and reconnection in protostellar disk formation in turbulent magnetized cores
TESTING MAGNETIC FIELD MODELS FOR THE CLASS 0 PROTOSTAR L1527