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首页> 外文期刊>The Astrophysical Journal. Letters >THE ORIGIN OF NON-MAXWELLIAN SOLAR WIND ELECTRON VELOCITY DISTRIBUTION FUNCTION: CONNECTION TO NANOFLARES IN THE SOLAR CORONA
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THE ORIGIN OF NON-MAXWELLIAN SOLAR WIND ELECTRON VELOCITY DISTRIBUTION FUNCTION: CONNECTION TO NANOFLARES IN THE SOLAR CORONA

机译：非最大世界太阳能通电电子速度分布功能的起源：与太阳能电晕的纳米粗罗拉连接

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The formation of the observed core-halo feature in the solar wind electron velocity distribution function is a longtime puzzle. In this Letter, based on the current knowledge of nanoflares, we show that the nanoflare-accelerated electron beams are likely to trigger a strong electron two-stream instability that generates kinetic Alfvén wave and whistler wave turbulence, as we demonstrated in a previous paper. We further show that the core-halo feature produced during the origin of kinetic turbulence is likely to originate in the inner corona and can be preserved as the solar wind escapes to space along open field lines. We formulate a set of equations to describe the heating processes observed in the simulation and show that the core-halo temperature ratio of the solar wind is insensitive to the initial conditions in the corona and is related to the core-halo density ratio of the solar wind and to the quasi-saturation property of the two-stream instability at the time when the exponential decay ends. This relation can be extended to the more general core-halo-strahl feature in the solar wind. The temperature ratio between the core and hot components is nearly independent of the heliospheric distance to the Sun. We show that the core-halo relative drift previously reported is a relic of the fully saturated two-stream instability. Our theoretical results are consistent with the observations while new tests for this model are provided.
机译：在太阳能通电分布函数中形成观察到的核心 - 光环特征是一个长时间拼图。在这封信中，根据目前的纳米闪闪发光的知识，我们表明纳米缺陷加速的电子束可能触发强的电子两流不稳定，其产生动力学Alfvén波和吹口波湍流，正如我们在前一篇论文中所示的那样。我们进一步表明，在动力湍流起源期间产生的核心 - 光环特征可能源于内电晕，并且可以保存，因为太阳风沿着开放的场线逸出到空间。我们制定一组方程来描述在模拟中观察到的加热过程，并表明太阳风的核心 - 光环温度比对电晕中的初始条件不敏感，并且与太阳能的核心 - 光环密度比有关风和对指数衰减结束时的两流不稳定性的准饱和度。这一关系可以扩展到太阳风中的更通用的核心晕 - Strahl特征。核心和热部件之间的温度比几乎与距太阳的灯光距离无关。我们表明，先前报道的核心 - 光环相对漂移是完全饱和的双流不稳定的遗物。我们的理论结果与观察结果一致，同时提供了该模型的新测试。

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