标题： 喷射出的高能电子前沿的等离子体不稳定性与III型太阳射电爆发 显示英文标题

标题： Plasma instability in the front of ejected energetic electrons and Type III solar radiobursts

摘要： III型射电爆发是太阳耀斑期间喷射出的近相对论电子通量的特征。 这些爆发经常被如帕克太阳探测器等航天器观测到。 传统上认为，这些电子束通过双流不稳定性产生朗缪尔波，然后转化为电磁波。 在本研究中，我们通过检查电子分布由于“飞行时间”效应在通过随机不均匀且缓慢变化的日冕物质中传播时如何被截断，从而修正了该模型。 而不是双流不稳定性，这种截断使分布不稳定，并通过线性不稳定性产生朗缪尔波；我们的分析局限于这个线性区域，并不考虑所产生的朗缪尔波对电子分布的非线性反作用。 不稳定性持续增长，直到较慢的电子到达并衰减波。 我们的定性分析表明，产生的波强度的增长和衰减与观测到的III型射电爆发在基频下的强度-时间曲线非常吻合，支持这一修正理论。 显示英文摘要

摘要： Type III radio bursts are a signature of the flux of near-relativistic electrons ejected during solar flares. These bursts are frequently observed by spacecraft such as the Parker Solar Probe. It is traditionally believed that these electron beams generate Langmuir waves through the two-stream instability, which are then converted into electromagnetic waves. In this study, we revise that model by examining how the electron distribution becomes truncated due to the "time-of-flight" effect as the beam travels through a randomly inhomogeneous, and gently varying solar-wind plasma. Rather than the two-stream instability, this truncation destabilizes the distribution and leads to the generation of Langmuir waves via a linear instability; we confine our analysis to this linear regime and do not take into account the back reaction of the generated Langmuir waves on the electron distribution, which is nonlinear. The instability grows until slower electrons arrive and dampen the waves. Our qualitative analysis shows that the resulting wave intensity growth and decay closely match the intensity-time profile of observed Type III radio bursts at the fundamental frequency, supporting this modified theory.