Solar explosive activity throughout the evolution of the solar system
Solar explosive activity throughout the evolution of the solar system
复制标题
整个太阳系演化过程中的太阳爆炸活动
DOI：
--
复制
发表时间：
2016
期刊：
影响因子：
--
通讯作者：
R. Osten
中科院分区：
文献类型：
--
作者：
R. Osten
太阳变化的时间尺度从几秒到几十亿年不等。太阳上的爆炸事件涉及到原子结构的变化和随后的能量释放，与这种能量转换有关的过程发生在这些时间尺度中最短的时间。然而.爆炸事件的性质可以在太阳的进化过程中改变。本章涵盖了整个太阳系演化过程中爆炸事件的历史，重点是观察到的爆炸事件的表现形式以及我们可以通过研究它们学到什么。本系列其他卷中的章节（见表I.2）讨论了该主题的部分内容。第m卷第2章描述了类太阳恒星磁活动的长期演化，第t 1卷第5章讨论了太阳和恒星爆发、耀斑和jet等的观测。关于加速粒子辐射特征的描述（主要是应用于日冕）可以在第11卷第4章中找到，而第6章则处理日冕物质抛射和耀斑的模型。虽然本章的主要主题是这些爆炸性事件的演变的时间尺度上的变化性质，其他重要的恒星参数，如旋转速率，对流区深度的影响，以及双星对旋转弧的影响也讨论了在适当的地方。本章的重点是使用爆炸事件的事件驱动的讨论，记住参数如何随着一些关键的恒星参数而变化。这种处理是为了说明这些年龄范围的恒星中已知的爆炸事件的关键特性。爆炸事件由几个不同的组成部分组成，从高能粒子到日冕物质抛射再到耀斑。在太阳上，这三种成分可以单独研究，而在太阳以外的恒星上，爆炸事件的识别和研究仅限于事件的辐射表现，即恒星耀斑。根据太阳的诊断，耀斑涉及粒子加速和等离子体加热。它们的出现是由于
The time scales on which the Sun varies range from seconds to billions of years. Explosive events on the Sun involve the changing of rnagncLic configurations and subsequent liberation of energy, and processes associated with thi s energy transformation occur on the shortest of these time scales. However. the nature of the explosive events can change over the course of the Sun'c; evolutionary lifetime. This chapte r covers the history of explosive events throughout the evolution of the solar system, with a focus on Lhe observed manifestations of explosive events and what we can learn by studying them. Chapters in other volumes of this series (see Table I .2) address parts of this topic. Chapter 2 of Vol. m describes the longterm evolution of magnetic activity of Sun-like stars, and Ch. 5 of Vol. Tl di scusses observations of solar and stelJar eruptions, flares, and jetc;. A description of radiative signatures of accelerated panicles (primarily with application to <;olar llares) can be found in Ch. 4 of Vol. 11, while Ch. 6 of that volume tackles models of coronal mass ejections and flares. While the mai n theme of this chapter is the changing nature of these explosive events over evolucionary time scales, the influence of other important stellar parameters such as rotation rate, convection zone depth, and the influence of binaricy on rotation arc also discussed where appropriate. The focus of the chapter is to use an event-driven discussion of explosive events, keeping in mind how the parameters change with some key stellar parameters. This treatment is meant to illustrate key properties of explosive events that are known in stars of these age ranges. An explosive event is made up of several distinct components, from energetic particles to coronal mass ejections to flares. While on the Sun these three components can be studied separate ly, on stars other than the Sun the identification and study of explosive events is limited to the radiative manifestation of the event, namely stellar flares. As diagnosed from the Sun, flares involve particle acceleration and plasma heating. They occur as a consequence of magnetic