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Influence Of Density Stratification On Solar Convection (Solar Studies)

密度分层对太阳对流的影响（太阳研究）

基本信息

批准号：
ST/X001083/1
负责人：
Laura Currie
金额：
$ 30.6万
依托单位：
Durham University
依托单位国家：
英国
项目类别：
Research Grant
财政年份：
2023
资助国家：
英国
起止时间：
2023 至无数据
项目状态：
未结题

来源：
https://gtr.ukri.org/projects?ref=ST%2FX001083%2F1
关键词：
Influence Density Stratification Solar Convection

项目摘要

The outer 30% of the Sun by radius is convecting. In this region, thermal gradients cause the fluid plasma to overturn. Currently, observations do not agree on the size of these convective motions and furthermore, discrepancies also occur between observations and numerical models of the Sun. This research project aims to address the uncertainty surrounding the length scale and amplitude of motions in the convection zone. This work also aims to shed light on how large-scale, convection-driven flows impact heat transport in the Sun and what the consequences of this are for the interior dynamics. Understanding the dynamics of the solar convection zone is crucial in understanding how the Sun builds its magnetic field through dynamo action. The Sun's magnetic field has a direct impact on Earth through space weather events such as solar storms which can disrupt satellite communications and power grids, and so a better understanding of the solar dynamo is key to predicting space weather events. To achieve these aims, two important physical aspects of the Sun must be considered. Namely, that it is rotating, and that its density drops off significantly over its depth. In this project, using a series of numerical simulations, we will investigate the important effects of rotation and density stratification and determine how key convective quantities scale with rotation rate in the presence of significant density stratification. We expect the depth-dependence introduced by density stratification to be fundamental in determining the heat transport and size of convection motions throughout the solar convection zone.

太阳半径外部 30% 的区域是对流区域。在该区域中，热梯度导致流体等离子体翻转。目前，观测结果对这些对流运动的大小并不一致，此外，观测结果与太阳数值模型之间也存在差异。该研究项目旨在解决对流区运动长度尺度和幅度的不确定性。这项工作还旨在揭示大规模对流驱动的流动如何影响太阳中的热传输以及这对内部动力学的影响。了解太阳对流区的动力学对于了解太阳如何通过发电机作用建立磁场至关重要。太阳磁场通过太阳风暴等空间天气事件对地球产生直接影响，太阳风暴可能会扰乱卫星通信和电网，因此更好地了解太阳发电机是预测空间天气事件的关键。为了实现这些目标，必须考虑太阳的两个重要物理方面。也就是说，它正在旋转，并且其密度在其深度上显着下降。在该项目中，我们将使用一系列数值模拟来研究旋转和密度分层的重要影响，并确定在存在显着密度分层的情况下关键对流量如何随旋转速率变化。我们预计密度分层引入的深度依赖性对于确定整个太阳对流区的热传输和对流运动的大小至关重要。