Constraining the Structure and Dynamics of the Upper Layers of the Convective Zone Using Accurate High Spatial Degree Modes Derived from GONG Observations

我们的现代社会高度依赖于技术的所有关键活动，包括导航，商业，运输，通信，电力供应和安全。 作为一颗磁性星星，我们的太阳已经破坏了，并将继续威胁破坏这些依赖技术的活动。 为了减轻不可避免的风险，我们必须进一步了解耀斑和日冕物质抛射（CME）等事件背后的过程。 所有这些现象背后的太阳磁场来自太阳等离子体中存在的流动。 这些流动是通过太阳内部的能量传输产生的。 这个为期3年的研究项目预计将提高我们对太阳表面以下结构，动力学和流动的了解。 这个区域是了解和预测太阳活动的关键。 该研究项目不仅具有重要的学术研究，而且还承诺为我们的技术驱动的社会带来切实和具体的好处。这个为期3年的项目旨在利用日震技术更好地描述太阳近地表层（太阳内部最外层的5%）。 这项工作将有助于回答的一个关键问题是：太阳（和其他类似太阳的恒星）是如何变化的？ 利用日震学，项目小组将能够推断和限制太阳内部结构和动力学的变化，方法是将p模式（或压力模式）振荡的精确特征扩展到更高的空间程度，并跟踪其随时间的变化。 该项目的技术方面是导出高阶模式的准确特征，即，使用国家统计局全球振荡网络组的观测结果，对200-900度范围内的球谐模频率、线宽、不对称性和振幅进行精确和无偏估计。 即将开展的研究工作将提高由NSF支持的GONG使命的科学回报。 因此，该项目支持AGS部门在发现，学习，多样性和跨学科研究方面的战略目标。

Our modern society is highly dependent on technology for all of its critical activities, including navigation, commerce, transportation, communication, power provision, and security. As a magnetic star, our Sun has disrupted, and will continue to threaten disrupting, these technology-dependent activities. In order to mitigate the inevitable risks, it is vital that we advance our understanding of the processes behind events such as flares and coronal mass ejections (CME). The solar magnetic field that underlies all of these phenomena arises from the flows present in the solar plasma. These flows are produced by the transport of energy through the solar interior. This 3-year research project is expected to improve our knowledge of the structure, dynamics and flows immediately below the surface of the Sun. This region is key to understanding and predicting solar activity. This research project features not only important academic research, but also promises a tangible and concrete benefit to our technologically powered society.This 3-year project is aimed at a better characterization of the Sun's near-surface layers (outermost 5% of the solar interior) using helioseismic techniques. A key question that this work will contribute to answering is: how and why does the Sun (and other Sun-like stars) vary? Using helioseismology, the project team will be able to infer and constrain changes in the structure and dynamics of the solar interior by extending the precise characterization of p-mode (or pressure-mode) oscillations to higher spatial degrees and tracking their changes with time. The technical aspect of this project is to derive accurate characteristics of high-degree modes, i.e., precise and unbiased estimates of mode frequency, line width, asymmetry and amplitude for spherical harmonics degrees in the range 200-900, using NSO's Global Oscillations Network Group (GONG) observations. The research work to be carried out would enhance the scientific return of the GONG mission, which has been supported by the NSF. Therefore, the project supports the Strategic Goals of the AGS Division in discovery, learning, diversity, and interdisciplinary research.