太阳耀斑中的准周期脉动：太阳能量释放的关键诊断
Quasi-periodic pulsations in solar flares: a key diagnostic of energy release on the Sun
摘要：
太阳耀斑是我们太阳系中最强大和最具破坏性的事件之一，然而驱动和传输这种能量释放的物理机制尚未完全了解。与耀斑能量释放相关的一个重要特征是在亚秒至分钟的时间尺度上高度可变的发射，其通常表现出振荡行为，统称为准周期性脉动（QPP）的特征。为了充分确定QPP的驱动机制，开发其作为诊断工具的潜力，并将其纳入我们对太阳和恒星耀斑的理解，需要新的观测能力和举措。显然，社区需要对太阳进行以耀斑为焦点、节奏快、分辨率高、多波长的成像，并具有足够高的灵敏度和动态范围，以便在总强度很大的情况下观测强度的微小波动。此外，需要多学科的资金和举措，以缩小数值模型和观测之间的差距。QPP是发生在耀斑磁重联和能量释放站点的物理的直接签名，因此是至关重要的，包括在一个统一的耀斑模型。尽管有大量的建模和理论工作，没有一个单一的机制或模型可以完全解释耀斑中QPP的存在。此外，QPP也可能属于不同机制产生的不同类别。目前，我们没有足够的信息来观察区分机制。耀斑对地球电离层的地球效应，以及恒星耀斑表现出类似的QPP特征，加强了理解QPP的动机。QPP提供了一个黄金机会，以更好地了解耀斑物理学和利用太阳恒星的类比，有利于天体物理学，太阳物理学和日地联系。
英文摘要：
Solar flares are among the most powerful and disruptive events in our solar system, however the physical mechanisms driving and transporting this energetic release are not fully understood. An important signature associated with flare energy release is highly variable emission on timescales of sub-seconds to minutes which often exhibit oscillatory behaviour, features collectively known as quasi-periodic pulsations (QPPs). To fully identify the driving mechanism of QPPs, exploit their potential as a diagnostic tool, and incorporate them into our understanding of solar and stellar flares, new observational capabilities and initiatives are required. There is a clear community need for flare-focused, rapid cadence, high resolution, multi-wavelength imaging of the Sun, with high enough sensitivity and dynamic range to observe small fluctuations in intensity in the presence of a large overall intensity. Furthermore, multidisciplinary funding and initiatives are required to narrow the gap between numerical models and observations. QPPs are direct signatures of the physics occurring in flare magnetic reconnection and energy release sites and hence are critical to include in a unified flare model. Despite significant modelling and theoretical work, no single mechanism or model can fully explain the presence of QPPs in flares. Moreover, it is also likely that QPPs fall into different categories that are produced by different mechanisms. At present we have insufficient information to observationally distinguish between mechanisms. The motivation to understand QPPs is strengthened by the geo-effectiveness of flares on the Earth's ionosphere, and by the fact that stellar flares exhibit similar QPP signatures. QPPs present a golden opportunity to better understand flare physics and exploit the solar-stellary analogy, benefiting both astrophysics, heliophysics, and the solar-terrestrial connection.
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