| Issue |
A&A
Volume 480, Number 1, March II 2008
|
|
|---|---|---|
| Page(s) | 27 - 33 | |
| Section | Astrophysical processes | |
| DOI | https://doi.org/10.1051/0004-6361:20077562 | |
| Published online | 02 January 2008 | |
Magnetic shear-driven instability and turbulent mixing in magnetized protostellar disks
1
INAF – Osservatorio Astrofisico di Catania, via S. Sofia 78, 95123 Catania, Italy e-mail: abo@oact.inaf.it
2
INFN, Sezione di Catania, via S. Sofia 72, 95123 Catania, Italy
3
A.F. Ioffe Institute of Physics and Technology and Isaac Newton Institute of Chile, Branch in St. Petersburg, 194021 St. Petersburg, Russia
Received:
28
March
2007
Accepted:
5
December
2007
Context.Observations of protostellar disks indicate the presence of the magnetic field of thermal (or superthermal) strength. In such a strong magnetic field, many MHD instabilities responsible for turbulent transport of the angular momentum are suppressed.
Aims.We consider the shear-driven instability that can occur in protostellar disks even if the field is superthermal.
Methods.This instability is caused by the combined influence of shear and compressibility in a magnetized gas and can be an efficient mechanism to generate turbulence in disks.
Results.The typical growth time is of the order of several rotation periods.
Key words: accretion, accretion disks / magnetohydrodynamics (MHD) / instabilities / turbulence / stars: formation
© ESO, 2008
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