期刊
PHYSICAL REVIEW E
卷 80, 期 6, 页码 -出版社
AMER PHYSICAL SOC
DOI: 10.1103/PhysRevE.80.066303
关键词
accretion disks; astrophysical fluid dynamics; black holes; Couette flow; flow instability; hydrodynamics; magnetic field effects; magnetohydrodynamics; star formation; turbulence
资金
- German Leibniz Gemeinschaft
- Deutsche Forschungsgemeinschaft [SFB 609]
- Science and Technology Facilities Council [PP/E001092/1] Funding Source: researchfish
- STFC [PP/E001092/1] Funding Source: UKRI
The magnetorotational instability (MRI) is thought to play a key role in the formation of stars and black holes by sustaining the turbulence in hydrodynamically stable Keplerian accretion disks. In previous experiments the MRI was observed in a liquid metal Taylor-Couette flow at moderate Reynolds numbers by applying a helical magnetic field. The observation of this helical MRI (HMRI) was interfered with a significant Ekman pumping driven by solid end caps that confined the instability only to a part of the Taylor-Couette cell. This paper describes the observation of the HMRI in an improved Taylor-Couette setup with the Ekman pumping significantly reduced by using split end caps. The HMRI, which now spreads over the whole height of the cell, appears much sharper and in better agreement with numerical predictions. By analyzing various parameter dependencies we conclude that the observed HMRI represents a self-sustained global instability rather than a noise-sustained convective one.
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