Quantutative MHD Modeling of the Solar Transition Region Using Realistic Transport Coefficients

ATM9816335abs研究人员将继续开发太阳过渡区的磁流体动力学（MHD）模型。 过渡区将太阳色球层和日冕分开。 它是一个薄的界面，一个不连续的，在较冷的部分电离的色球层和热得多的完全电离的日冕之间。 极紫外太阳光谱的很大一部分来自过渡区。 为了确定过渡区是如何被加热的，有必要将联合收割机观测结果与模型相结合，该模型预测描述过渡区的参数空间区域中的能量耗散和热能传输速率。 在MHD模型中，这意味着必须在表征过渡区的温度、密度、速度和磁场范围内使用和评估确定电阻和粘性耗散率以及热能通量的传输系数的现实表达式。 由于目前的限制，在计算机速度，多维，时间相关的MHD模拟不能使用这些传输系数，甚至远程现实值。 研究人员将对现有的MHD模型进行修改，以包括粘性效应，电子和质子的单独能量方程，以及电子温度和密度方面的净辐射损失的参数表示。 该模型将有助于解决的争议，以何种程度的过渡区加热原位粘性耗散，耗散的传导和热电流，相比，通量的热能从上覆的日冕

ATM9816335absThe investigators will continue the development of a magnetohydrodynamic (MHD) model of the solar transition region. The transition region separates the solar chromosphere and the solar corona. It is a thin interface, a discontinuity, between the cooler, partially ionized chromosphere and the much hotter fully ionized corona. A large part of the extreme ultraviolet solar spectrum comes from the transition regions. In order to determine how the transition region is heated, it is necessary to combine observations with models that predict energy dissipation and thermal energy transport rates in the region of parameter space that describes the transition region. In an MHD model, this means that realistic expressions for the transport coefficients that determine resistive and viscous dissipation rates and thermal energy flux must be used, and evaluated, in the ranges of temperature, density, velocity, and magnetic field that characterize the transition region. Due to current limitations in computer speed, multi-dimensional, time dependent MHD simulations cannot use even remotely realistic values of these transport coefficients. The investigators will make modifications to an existing MHD model to include viscous effects, separate energy equations for electrons and protons, and a parametric representation of the net radiative loss in terms of electron temperature and density. The model will help resolve the controversy as to what degree the transition region is heated by in situ viscous dissipation, and dissipation of conduction and thermoelectric currents, as compared to the flux of thermal energy from the overlying corona