Newly Discovered Source of Turbulence and Heating in the Solar Chromosphere
Newly Discovered Source of Turbulence and Heating in the Solar Chromosphere
复制标题
DOI：
10.3847/2041-8213/ab75bc
复制
发表时间：
2020-02
期刊：
影响因子：
--
通讯作者：
M. Oppenheim;Y. Dimant;W. Longley;A. Fletcher
中科院分区：
文献类型：
--
作者：
M. Oppenheim;Y. Dimant;W. Longley;A. Fletcher
在太阳发光的光球层之上是太阳色球层，那里的温度从低于4000 K上升到超过100万K。虽然物理学家不明白这些增加的来源，但他们知道它为太阳风提供动力，对整个太阳系产生巨大影响。本报告描述了一组模拟和分析理论，表明起源于光球层的太阳大气流将经常驱动先前未识别的热等离子体不稳定性，并迅速发展成湍流。虽然这种湍流的尺度很小（厘米到几米），但它会改变色球层的电导率，温度和能量流。将这种湍流和其他小尺度湍流的影响应用到太阳和恒星大气的大尺度模型中，将提高物理学家模拟能量流的能力，并对预测的温度和辐射模式产生重要影响。
Above the Sun’s luminous photosphere lies the solar chromosphere, where the temperature increases from below 4000 K to over 1 million K. Though physicists do not understand the origin of these increases, they know it powers the solar wind with enormous consequences for the entire solar system. This report describes a set of simulations and analytical theory showing that solar atmospheric flows originating in the photosphere will frequently drive a previously unidentified thermal plasma instability that rapidly develops into turbulence. Though this turbulence is small scale (centimeters to a few meters), it will modify the conductivity, temperatures, and energy flows through much of the chromosphere. Incorporating the effects of this turbulence, and other small-scale turbulence, into large-scale models of solar and stellar atmospheres will improve physicists’ ability to model energy flows with important consequences for the predicted temperatures and radiation patterns.