太阳磁场的自组织
Self-organization of solar magnetic fields
摘要：
持续磁化等离子体的自组织特性被应用到选定的太阳数据，以了解太阳磁场。扭转振荡是与太阳活动周期相关的方位流的加速和减速带，它们意味着存在一个对称的太阳发电机，测得的极通量为3 × 10^14 Wb。结果表明，太阳发电机是薄的（~0.1微米梯度尺度大小）和强大的（~10^23 W）。这些特性是从扭转振荡的振幅和它们的速度等值线与太阳磁图的关系中发现的。发电机有足够的能量来加热色球层，并为日冕和太阳风提供能量。发电机也会导致日光层的刚性旋转，至少到日冕，日冕旋转与太阳磁图的关系也支持这一结果。薄薄的太阳发电机维持着薄薄的稳定的最低能量状态，似乎覆盖了光球层下方的大部分太阳表面。最低能态的磁力线应平行于太阳表面，并随着离太阳表面的距离以2π弧度的旋转在~1 μ m内旋转。电阻性扩散有助于将磁场推到表面，全球磁结构（GMS）似乎每11年失去π弧度，导致观测到的太阳磁场180度翻转。太阳黑子中的磁化等离子体薄片可能是GMS失去的薄片。为了完整起见，讨论了太阳黑子、日冕物质抛射和耀斑的形成。
英文摘要：
Self-organization properties of sustained magnetized plasma are applied to selected solar data to understand solar magnetic fields. Torsional oscillations are speed-up and slow-down bands of the azimuthal flow that correlate with the solar cycle, and they imply the existence of a symmetric solar dynamo with a measured polar flux of 3x10^14 Wb. It is shown that the solar dynamo is thin (~0.1 Mm gradient scale size) and powerful (~10^23 W). These properties are found from the amplitude of the torsional oscillations and the relationship of their velocity contours to solar magnetograms supports the result. The dynamo has enough power to heat the chromosphere and to power the corona and the solar wind. The dynamo also causes a rigid rotation of the heliosphere out to at least the corona and the relationship of the rotation of the corona to solar magnetograms supports this result as well. The thin solar dynamo sustains a thin stable minimum energy state that seems to be covering most of the solar surface just below the photosphere. The magnetic field lines of the minimum energy state should be parallel to the solar surface and rotate with distance from the surface with 2π radians of rotation in ~1 Mm Resistive diffusion helps to push the magnetic fields to the surface and the global magnetic structure (GMS) seems to lose π radians every 11 years, causing the observed 180 degree flipping of the solar magnetic field. The thin sheets of magnetized plasma in solar prominences may be the lost thin sheets of the GMS. For completeness, the formation of sunspots, CMEs and flares is discussed.
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