Coronal Magnetography of Solar Active Regions via 3D Modeling and Radio Imaging Spectroscopy

首席研究员（PI）和他的团队将通过先进的理论发展和陀螺共振（GR）和自由发射的3D建模，研究太阳活动区无线电成像光谱观测的使用和解释。GR过程允许无线电发射提供日冕磁场强度和方向的直接测量，因此提供了理解所有太阳活动的基本机制的关键。该小组最近将空间和光谱分辨的无线电发射与光球磁图和其他数据的磁场外推进行了比较，这表明可能需要将现有理论扩展到非麦克斯韦粒子分布，以解释观测到的太阳无线电源高度。因此，PI将开发一个全面的模型框架，能够再现物理上真实的太阳大气结构，包括非热粒子的分布。PI现有的工具已经成功地计算了回旋同步加速器（GS）无线电发射和硬X射线发射，用于太阳耀斑的前向拟合微波和X射线观测。在这里，该团队计划修改这个通用框架来模拟GR排放。这需要单独的开发工作来处理GR过程中产生的特定问题，包括网格分辨率问题、在球坐标中处理该过程以处理活动区域发射所涉及的大视场，以及开发一致的方法来指定环境太阳等离子体温度和密度以及磁场。在这项工作中，PI的团队将为太阳和空间气象界开发用户友好的软件工具，然后通过SolarSoft软件分发库在网上广泛传播。由于这项工作将在新泽西理工学院（NJIT）的日地研究中心进行，该活动将促进发现和理解，同时促进教学，培训和学习。PI计划将这里开发的分析工具整合到NJIT的研究生课程中，包括射电天文学，太阳物理学和等离子体物理学的课程。鉴于磁场和等离子体粒子分布在天体物理学研究中至关重要，这项研究也将广泛适用于太阳物理学之外。

The Principal Investigator (PI) and his team will investigate the use and interpretation of radio imaging spectroscopy observations of solar active regions through advanced theory development and 3D modeling of gyroresonance (GR) and free-free emission. The GR process permits radio emission to provide direct measurements of magnetic field strength and direction in the solar corona, and so supplies the key to understanding the basic mechanisms underlying all of solar activity. This team's recent work in comparing spatially and spectrally resolved radio emission with magnetic field extrapolations of photospheric magnetograms and other data has suggested that an extension of existing theory to non-Maxwellian particle distributions may be needed to account for the observed altitudes of solar radio sources. The PI therefore will develop a comprehensive modeling framework for flaring loops that is capable of reproducing physically realistic solar atmospheric structure, including distributions of non-thermal particles. The PI's existing tools have already successfully calculated both gyrosynchrotron (GS) radio emission and hard X-ray emission for forward-fitting microwave and X-ray observations of solar flares. Here, the team plans to modify this general framework to model GR emission. This requires a separate development effort to deal with specific issues arising from the GR process, including grid resolution problems, the treatment of the process in spherical coordinates to deal with the large fields of view involved in active region emission, and the development of a consistent way to specify ambient solar plasma temperature and density in addition to the magnetic field. In this effort, the PI's team will develop user-friendly software tools for the solar and space weather community, and then widely disseminate them online through the SolarSoft software distribution library. Since this work will be performed at the Center for Solar-Terrestrial Research at the New Jersey Institute of Technology (NJIT), the activity will advance discovery and understanding while promoting teaching, training, and learning. The PI plans to integrate the analysis tools developed here into graduate courses at NJIT, including curricula in radio astronomy, solar physics, and plasma physics. This research will also broadly be applicable beyond solar physics, given that both magnetic fields and plasma particle distributions are fundamentally important in astrophysics studies.