热太阳大气中漂移回旋加速器模的增长
Growing drift-cyclotron modes in the hot solar atmosphere
摘要：
众所周知的分析结果处理离子回旋和漂移波，并遵循从动力学理论和色散方程，它描述了耦合的两种模式，数值求解。利用适用于日冕的等离子体密度、磁场和温度值获得的数值结果清楚地表明了两种模式的耦合和不稳定性（增长）。耦合发生在非常短的波长，这是离子陀螺半径的顺序，并为特征尺度长度的平衡密度是高度相关的，可能成为只有几米的顺序。通过使用严格的动力学理论模型和现实的参数值得到的两个耦合模式（由平衡密度梯度驱动）的证明不稳定性。耦合背后的物理机制很简单，预计将在整个太阳大气和太阳风中发生，太阳大气和太阳风包含各种尺寸的非常细长的密度结构。该模式由于密度梯度而增长，它本质上是离子模式，并且其进一步耗散应导致增加的离子加热。
英文摘要：
Well-known analytical results dealing with ion cyclotron and drift waves and which follow from the kinetic theory are used and the dispersion equation, which describes coupled two modes, is solved numerically. The numerical results obtained by using the values for the plasma density, magnetic field and temperature applicable to the solar corona clearly show the coupling and the instability (growing) of the two modes. The coupling happens at very short wavelengths, that are of the order of the ion gyro radius, and for characteristic scale lengths of the equilibrium density that are altitude dependent and may become of the order of only a few meters. The demonstrated instability of the two coupled modes (driven by the equilibrium density gradient) is obtained by using a rigorous kinetic theory model and for realistic parameter values. The physical mechanism which is behind the coupling is simple and is expected to take place throughout the solar atmosphere and the solar wind which contain a variety of very elongated density structures of various sizes. The mode grows on account of the density gradient, it is essentially an ion mode, and its further dissipation should result in an increased ion heating.
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