发表机构
Università di Palermo; INAF-Osservatorio Astronomico di Palermo; Harvard–Smithsonian Center for Astrophysics（巴勒莫大学; 意大利国家天体物理研究所巴勒莫天文台; 哈佛-史密松尼天体物理中心）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本文通过MHD模拟研究磁重联产生的纳米耀斑加热与纳米喷流特性，发现喷流性质可揭示重联信息，但加热量与喷流速度关联困难，模型可解释多种加热事件。
AI 中文摘要
磁重联被视为解释太阳日冕持续且爆发性加热（从而维持其热结构）的主要机制。近年来，对磁重联外流（即纳米喷流）的观测与建模增强了我们审视该机制的能力，然而，关于能量事件与运动学事件之间关系仍需更多理解。本文旨在详细研究加热事件（纳米耀斑）及其运动学对应物（纳米喷流）的性质，以增强对磁重联事件的探测能力。我们使用两个磁通量管相互作用的MHD模拟，其中发生磁重联并产生此类重联外流。我们改变关键参数，如临界电流和计算域尺寸，以研究加热机制和弹弓机制。我们发现，纳米喷流的性质可以透露许多关于产生它的磁重联的信息，而加热量级与喷流速度之间难以直接关联。我们还发现，此类重联模型可以解释广泛的加热事件。磁重联仍然与加热和外流密不可分，我们的模拟展示了这两种磁重联副产物之间复杂的相互作用，以及如何通过观测研究它们的性质。
英文摘要
Magnetic reconnection is seen as the lead mechanism to explain the persistent and bursty heating of the solar corona that keeps its thermal structure. Lately the observations and modelling of magnetic reconnection outflows, i.e. nanojets, has empowered our capabilities to scrutinise this mechanisms, however more needs to be understood on the relation between the energetic and kinematic events. The aim of this paper is to study in details the properties of the heating events (nanoflare) and the kinematic counterparts (nanojets) in order to augment detection capabilities of magnetic reconnection events. We use MHD simulations of the interaction of two magnetic flux tubes where magnetic reconnection occurs and such reconnection outflows are generated. We vary key parameters, such as the critical current and the size of the domain to study the heating and slingshot mechanisms. We find that the properties of the nanojets can give away much information on the magnetic reconnection that generated it, while it is difficult to directly link the amount of heating and the jet speeds. We also find that such reconnection model can explain a wide range of heating events. Magnetic reconnection still is invariably linked to both heating and outflows and our simulations show the complex interplay between these two byproducts of the magnetic reconnection and how their properties can be studied in observations.
