The Physics of Wave Dynamics in the Solar Atmosphere

太阳大气中波动力学的物理学

• 批准号: 2108185
• 金额: --
• 依托单位: University of Warwick
• 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-2108185
• 关键词: Physics; Wave; Dynamics; Solar; Atmosphere

Abstract:The atmosphere of the Sun above the visible surface (photosphere) is divided in several distinct layers that include the chromosphere, transition region and corona. These layers are highly dynamic with exchange of matter and energy. It is still not clear what maintains the atmospheric temperatures against radiative losses - the so called heating problem. It is believed that waves have an important role in delivering energy from surface convection into the atmosphere, and may also cause cool chromospheric material to be launched up into the corona (resembling observed spicules). Furthermore, waves are seen in structures at all temperatures and play a part in the cooling process of coronal plasma (oscillating rain). In this project, we shall examine the role of waves at the physical interface between hot (coronal) and cool (chromospheric) plasmas. It will involve a combination of theory, observations and numerical simulation. It will use codes developed at Warwick (Lare3D) and data from the solar satellites Hinode, IRIS and SDO along with data from the DKIST ground based telescope due to begin operation in 2019.Potential impact:Out understanding of wave coupling will further our understanding of the problem of how the solar atmosphere is heated. Large-amplitude oscillations will provide insight into solar flares and coronal mass ejections, which are sources of space weather.Aims and objectives:A combined observational and theoretical (numerical) approach to further our understanding of the physical conditions for wave coupling between the various layers of the solar atmosphere.Novelty:We will be using the improved facilities of the Warwick 3d MHD code Lare3D, which now included efficient thermal conduction and radiative losses to better model wave propagation in the solar chromosphere. We shall combine observations from AIA and IRIS to look for oscillatory signatures that span both chromosphere and corona, which will also be preparatory work for the DKIST observatory that will come online in 2019.

摘要：太阳可见表面（光球层）以上的大气被划分为几个不同的层，包括色球层、过渡区和日冕。随着物质和能量的交换，这些层是高度动态的。目前还不清楚是什么维持了大气温度，使其不受辐射损失的影响——即所谓的加热问题。据信，波在将能量从表面对流输送到大气中起着重要作用，也可能导致冷色球物质被发射到日冕中（类似于观察到的针状体）。此外，在任何温度的结构中都可以看到波，并在日冕等离子体（振荡雨）的冷却过程中发挥作用。在这个项目中，我们将研究波在热（日冕）和冷（色球）等离子体之间的物理界面上的作用。它将包括理论、观测和数值模拟的结合。它将使用沃里克开发的代码（Lare3D）和来自太阳卫星Hinode、IRIS和SDO的数据，以及将于2019年开始运行的DKIST地面望远镜的数据。潜在影响：我们对波耦合的理解将进一步加深我们对太阳大气如何被加热问题的理解。大振幅振荡将提供深入了解太阳耀斑和日冕物质抛射，这是空间天气的来源。目的和目标：结合观测和理论（数值）方法，进一步了解太阳大气各层之间波耦合的物理条件。新颖性：我们将使用Warwick 3d MHD代码Lare3D的改进设施，现在包括有效的热传导和辐射损失，以更好地模拟太阳色球中的波传播。我们将结合AIA和IRIS的观测，寻找跨越色球层和日冕的振荡特征，这也是将于2019年上线的DKIST天文台的准备工作。