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Energy release and transport in solar flares

太阳耀斑中的能量释放和传输

基本信息

批准号：
2049963
负责人：
金额：
--
依托单位：
University College London
依托单位国家：
英国
项目类别：
Studentship
财政年份：
2018
资助国家：
英国
起止时间：
2018 至无数据
项目状态：
已结题

来源：
https://gtr.ukri.org/projects?ref=studentship-2049963
关键词：
Energy release transport solar flares

项目摘要

The magnetic field of the corona not only stores the energy that is released during solar flares and coronal mass ejections (CMEs) but, as a consequence of the low plasma beta conditions, it both defines the reconnection environment, and plays a central role in the transport of this energy throughout the atmosphere. Indeed, different reconnection scenarios in different field configurations can lead to a variety of outcomes in terms of the evolution of the energy release and the efficiency of the energy transport mechanisms (via waves, particle acceleration and plasma heating). These variations manifest themselves as differences in the spatial, spectral and temporal properties of the electromagnetic signatures produced in the lower atmosphere, thus providing a means to quantify the effect of different field configurations on the energy release process. The 'standard' eruptive flare (CSHKP) model offers a framework in which to understand the global characteristics of the energy release. However, the factors that determine the primary method of energy transport and its efficiency remain controversial, fundamentally limiting our ability to understand what drives how energy is partitioned. It is the goal of this project to quantify the link between the properties, structure and connectivity of the reconnecting field, and how it determines the efficiency of the associated energy deposition in the lower solar atmosphere. Establishing this key relationship will provide new insights into the basic physics of the energy release, particle acceleration and transport processes in magnetised plasmas - the primary constituent of not just our solar system, but the universe.In order to achieve the project goals data from both space and ground-based assets will be utilised (Hinode, SDO, RHESSI, IRIS, SST, ROSA and DKIST) and combined with state-of-the art radiative hydrodynamic modelling codes, e.g. RADYN and HYDRO2GEN.

日冕的磁场不仅储存太阳耀斑和日冕物质抛射（CME）期间释放的能量，而且由于低等离子体β条件，它既定义了重联环境，又在整个大气层中传输该能量方面发挥着核心作用。事实上，不同场配置中的不同重连场景可能会导致能量释放演变和能量传输机制（通过波、粒子加速和等离子体加热）效率方面的各种结果。这些变化表现为低层大气中产生的电磁特征的空间、光谱和时间特性的差异，从而提供了一种量化不同场配置对能量释放过程的影响的方法。 “标准”喷发耀斑（CSHKP）模型提供了一个框架来了解能量释放的全球特征。然而，决定能源运输主要方式及其效率的因素仍然存在争议，从根本上限制了我们理解能源分配方式驱动因素的能力。该项目的目标是量化重新连接场的特性、结构和连通性之间的联系，以及它如何确定太阳低层大气中相关能量沉积的效率。建立这种关键关系将为磁化等离子体中能量释放、粒子加速和传输过程的基本物理提供新的见解——磁化等离子体不仅是我们太阳系的主要组成部分，也是宇宙的主要组成部分。为了实现项目目标，将利用来自空间和地面资产的数据（Hinode、SDO、RHESSI、IRIS、SST、ROSA 和 DKIST）并与最先进的辐射流体动力学相结合建模代码，例如RADYN 和 HYDRO2GEN。