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首页> 外文期刊>Plasma physics and controlled fusion >Thermal instability and non-equilibrium in solar coronal loops: from coronal rain to long-period intensity pulsations
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Thermal instability and non-equilibrium in solar coronal loops: from coronal rain to long-period intensity pulsations

机译：太阳能冠状环路中的热不稳定和非平衡：从冠状雨到长期强度脉动

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摘要

The complex interaction of the magnetic field with matter is the key to some of the most puzzling observed phenomena at multiple scales across the Universe, from tokamak plasma confinement experiments in the laboratory to the filamentary structure of the interstellar medium. A major astrophysical puzzle is the phenomenon of coronal heating, upon which the most external layer of the solar atmosphere, the corona, is sustained at multi-million degree temperatures on average. However, the corona also conceals a cooling problem. Indeed, recent observations indicate that, even more mysteriously, like snowflakes in the oven, the corona hosts large amounts of cool material termed coronal rain, hundreds of times colder and denser, that constitute the seed of the famous prominences. Numerical simulations have shown that this cold material does not stem from the inefficiency of coronal heating mechanisms, but results from the specific spatio-temporal properties of these. As such, a large fraction of coronal loops, the basic constituents of the solar corona, are suspected to be in a state of thermal non-equilibrium (TNE), characterised by heating (evaporation) and cooling (condensation) cycles whose telltale observational signatures are long-period intensity pulsations in hot lines and thermal instability-driven coronal rain in cool lines, both now ubiquitously observed. In this paper, we review this yet largely unexplored strong connection between the observed properties of hot and cool material in TNE and instability and the underlying coronal heating mechanisms. Focus is set on the long-observed coronal rain, for which significant research already exists, contrary to the recently discovered long-period intensity pulsations. We further identify the outstanding open questions in what constitutes a new, rapidly growing field of solar physics.
机译：磁场与物质的复杂相互作用是宇宙中多个尺度的一些最令人费解的观察现象的关键，从实验室中的Tokamak血浆监禁实验到壁球菌培养基的丝状结构。主要的天体物理拼图是冠状加热现象，在其上，太阳能大气层的最外部层，电晕，平均是在多百万度的温度下维持。然而，电晕还隐藏了一个冷却问题。事实上，最近的观察结果表明，甚至更神秘地像烤箱中的雪花一样，电晕占据了大量的酷材料，称为冠状雨，较冷和密集的数百次，这构成了着名突出的种子。数值模拟表明，这种冷材料不会源于冠状加热机制的低效率，而是由这些的特定时空性质产生。因此，大部分冠状环，太阳能电晕的基本成分被怀疑是在热非平衡（TNE）的状态下，其特征在于，通过加热（蒸发）和冷却（缩合）循环，其特征在于观察签名是热线中的长期强度脉动和凉爽线的热不稳定驱动的冠状雨，现在都普遍地观察到。在本文中，我们在TNE和不稳定性和潜在的冠状加热机制中观察到的热和凉料材的特性与潜在的冠状加热机制之间几乎不开发的强大联系。重点是在长期观察到的冠状雨上，这有重大研究已经存在，与最近发现的长期强度脉动相反。我们进一步确定了构成一个新的快速增长的太阳物理领域的未突出的开放问题。

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