期刊
ASTROPHYSICAL JOURNAL
卷 714, 期 2, 页码 1606-1616出版社
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/714/2/1606
关键词
magnetic fields; magnetohydrodynamics (MHD); Sun: photosphere; turbulence
资金
- Max-Planck Society
- Institute for Plasma Physics, Garching [MIF-IF-A-AERO8047]
We demonstrate that a magneto-convection simulation incorporating essential physical processes governing solar surface convection exhibits turbulent small-scale dynamo action. By presenting a derivation of the energy balance equation and transfer functions for compressible magnetohydrodynamics, we quantify the source of magnetic energy on a scale-by-scale basis. We rule out the two alternative mechanisms for the generation of the small-scale magnetic field in the simulations: the tangling of magnetic field lines associated with the turbulent cascade and Alfvenization of small-scale velocity fluctuations (turbulent induction). Instead, we find that the dominant source of small-scale magnetic energy is stretching by inertial-range fluid motions of small-scale magnetic field lines against the magnetic tension force to produce (against Ohmic dissipation) more small-scale magnetic field. The scales involved become smaller with increasing Reynolds number, which identifies the dynamo as a small-scale turbulent dynamo.
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