Nonlinear stability of solar type III radio bursts. I. Theory
Nonlinear stability of solar type III radio bursts. I. Theory
复制标题
太阳 III 型射电暴的非线性稳定性。
DOI：
10.1086/157502
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发表时间：
1979
期刊：
影响因子：
--
通讯作者：
K. Papadopoulos
中科院分区：
文献类型：
--
作者：
Robert A. Smith;M. Goldstein;K. Papadopoulos
提出了太阳III型爆发的激发理论。最初不稳定于线性尾撞不稳定性的电子可以迅速地将朗缪尔波放大到具有强烈湍流特征的能量密度。推导了描述强耦合(波-波)相互作用的三维方程。对于行星际介质的参数特征，方程简化为一维。在这种情况下，振荡双流不稳定性(OTSI)是主要的非线性不稳定性。OTSI通过产生非线性离子密度波动来稳定，这种波动有效地散射了与电子束共振的朗缪尔波。还建立了电子分布函数的解析模型，用于估算电子束从日冕传播到1AU及以上的总能量损失。
A theory of the excitation of solar type III bursts is presented. Electrons initially unstable to the linear bump-in-tail instability are shown to rapidly amplify Langmuir waves to energy densities characteristic of strong turbulence. The three-dimensional equations which describe the strong coupling (wave-wave) interactions are derived. For parameters characteristic of the interplanetary medium the equations reduce to one-dimension. In tha case the oscillating two-stream instability (OTSI) is the dominant nonlinear instability. OTSI is stabilized through the production of nonlinear ion density fluctuations that efficiently scatter Langmuir waves out of resonance with the electron beam. An analytical model of the electron distribution function is also developed which is used to estimate the total energy losses suffered by the electron beam as it propagates from the solar corona to 1 AU and beyond.