Buoyant Magnetic Fields in the Sun

太阳中的浮力磁场

• 批准号: 2281192
• 金额: --
• 依托单位: Newcastle University
• 依托单位国家: 英国
• 项目类别: Studentship
• 财政年份: 2019
• 资助国家: 英国
• 起止时间: 2019 至 无数据
• 项目状态: 已结题
• 来源: https://gtr.ukri.org/projects?ref=studentship-2281192
• 关键词: Buoyant; Magnetic; Fields; Sun

The subject of this project involves the physical processes governing the radial transport of magnetic fields in the solar interior. The interior of the Sun is generally divided into three main sections; the core (where energy is generated);the radiative zone and the convective zone so called because of the primary process by which heat is transferred. This project is concerned with the processes within the convective zone, where convection is the most signicant process of heat transport. It is believed that strong magnetic fields are generated at the base of the convective zone (or the tachocline). These magnetic fields "float" across the turbulent convective zone and appear at the surface (or photosphere) and are thought to be an important factor in the creation of sunspots, and coronal mass ejections. The project being undertaken here will look to better understand and model the process by which the magnetic fields move through the convective zone.The primary process we are trying to understand is called magnetic buoyancy. Magnetic buoyancy relies on the convection of plasma within the Sun. To model convection and hence magnetic buoyancy we need a compressible modelwhich allows for changes in density since convection relies on fluid parcels being of different densities and "floating" accordingly. However, another feature of compressible fluids (fluids in which density perturbations exist) is sound oracoustic waves. Sound waves are not of interest for this project because they are very computationally expensive to deal with. So one of the problems this project will seek to address is to find a model that can model magnetic buoyancywithout sound waves propagating - we call these models sound proof. Aims:* To compare different sound proof models and assess how accurately they model magnetic buoyancy.* Adapt an existing model or create a new model that models magnetic buoyancy in a way where sound waves are absent or of little consequence.1

该项目的主题涉及管理太阳内部磁场径向传输的物理过程。太阳内部通常分为三个主要部分：核心(产生能量的地方)、辐射区和对流区，因为热量传递的主要过程所以被称为辐射区和对流区。这个项目是关于对流区内的过程，在那里对流是最重要的热量传输过程。人们认为，强磁场产生于对流带(或斜长带)的底部。这些磁场“漂浮”在湍流对流区，并出现在表面(或光球层)，被认为是太阳黑子和日冕物质抛射产生的重要因素。这里正在进行的项目将寻求更好地了解磁场通过对流区的过程并建立模型。我们试图了解的主要过程称为磁浮力。磁浮力依赖于太阳内部等离子体的对流。为了模拟对流和磁浮力，我们需要一个可压缩的模型，它允许密度的变化，因为对流依赖于不同密度的流体粒子，并相应地“漂浮”。然而，可压缩流体(其中存在密度扰动的流体)的另一个特征是声波或声波。声波对这个项目不感兴趣，因为处理它们的计算成本非常高。因此，这个项目要解决的问题之一是找到一种模型，可以在没有声波传播的情况下模拟磁浮力--我们称这些模型为隔音模型。目标：*比较不同的隔音模型，并评估它们模拟磁浮力的精确度。*调整现有模型或创建一个新模型，在没有声波或影响很小的情况下模拟磁浮力。1