Alpha-Effect, Helicity and Angular Momentum Transport for a Magnetically Driven Turbulence in the Solar Convection Zone

摘要: For a given field of magnetic fluctuations the dynamo-α, as well kinetic and current helicities, have been computed, assuming that turbulence is subject to buoyancy global rotation. The sign dynamo-α positive in northern hemisphere negative southern hemisphere. helicity has just same latitudinal distribution α-effect, indeed there no minus between helicity. Also 〈j ⋅ B 〉 changes its at equator. It Our helicities (due fluctuations) α-effects are thus always out phase, this confirming previous result Keinigs (1983) Radler Seehafer (1990). signs α-effect both correspond numerical simulations by Brandenburg Schmitt (1998). We also computed turbulent angular momentum transport, which proves be inwards, hydrodynamic without fields (Chan, 1999). Thus we can easily explain why, supergranulation zone, deeper layers appear rotate faster than solar surface plasma, or why tachocline high-latitudes velocity decreases outwards. dynamo number derived from observed reveals rather small, unless eddy diffusivity not low sunspot decay suggests (i.e., 1011 cm2 s−1).