SHINE: Testing Theories of Coronal Heating and Solar Wind Acceleration with Multi-Messenger Data and Four-Dimension (4D) Forward Modeling

了解日冕的复杂性和演变是能够预测太阳对地球局部空间环境影响的必要前提。尽管经过多年的研究，我们仍然不知道加热日冕和加速太阳风的基本物理过程。该项目结合了数值模拟和数据分析，以更好地了解这些过程。一名研究生和一名本科生将得到支持和指导。拟议调查的目标是大大缩小已建议在太阳大气层外沿着封闭和开放磁场线激发等离子体的过程清单。这项工作设计了一个前向建模框架，该框架包括尽可能多的过程，所有过程都处于平等地位，并利用可用的“多信使”数据（即，（遥感和现场），以限制造成日冕加热和太阳风加速的物理过程的相对作用。具体而言，研究包括四个核心任务：（1）构建低日冕EUV和X射线发射的视线前向模型，对应于尽可能广泛的加热理论。(2)应用六种不同的磁力线外推模式由光球下边界条件计算日冕磁场。(3)通过对共转相互作用区（CIR）和湍流场线随机游走的形成进行高分辨率模拟，确定日冕通量管结构的哪些水平可以在行星际空间中被探测到。(4)使用新一代现有代码对沿沿着开放通量管的日冕加热和太阳风加速进行自洽建模，该代码现在包括波/湍流和交换重连物理学。该奖项反映了NSF的法定使命，并通过使用基金会的知识价值和更广泛的影响审查标准进行评估，被认为值得支持。

Understanding the complexity and evolution of the solar corona is a necessary precursor to being able to predict the Sun’s effects on the Earth’s local space environment. Despite many years of study, the basic physical processes responsible for heating the solar corona and accelerating the solar wind are still not known. This project combines numerical simulations and data analysis to better understand these processes. A graduate student and undergraduate students will be supported and mentored.The goal of the proposed investigation is to substantially narrow down the list of processes that have been suggested for energizing plasma along both closed and open magnetic field lines in the outer solar atmosphere. This work designs a forward-modeling framework that includes as many of the processes as possible, all on equal footing and takes advantage of the available “multi-messenger” data (i.e., both remote-sensing and in situ) to put constraints on the relative contributions of the physical processes responsible for coronal heating and solar wind acceleration. Specifically, the investigation consists of four core tasks: (1) Constructing line-of-sight forward models of EUV and X-ray emission for the low corona, corresponding to as broad a range of proposed heating theories as possible. (2) Implementing six different field-line extrapolation models to compute the coronal magnetic field from photospheric lower boundary conditions. (3) Determining what levels of coronal flux-tube structure can survive to be detectable in interplanetary space, through high-resolution simulations of the formation of corotating interaction regions (CIRs) and turbulent field-line random walk. (4) Self-consistent modeling of coronal heating and solar wind acceleration along open flux tubes using a new generation of an existing code that now includes both wave/turbulence and interchange reconnection physics.This award reflects NSF's statutory mission and has been deemed worthy of support through evaluation using the Foundation's intellectual merit and broader impacts review criteria.