Identifying Magnetohydrodynamic Mechanisms of Chromospheric Heating and Flow Generation Using Models with a Realistic Description of Transport Processes

将开发两个磁流体动力学模型，以研究太阳和恒星大气中的非热加热、定向等离子体流的产生以及高能粒子加速过程。 这两个模拟的一个关键组成部分将是一个现实的传输过程中的各向异性张量的电导率和热导率，以及粘度的形式描述。 当磁化等离子体既不处于无碰撞状态，也不处于碰撞主导状态时，这种处理是必要的。 一个模型将描述小振幅波在两个空间维度中的传播，特别强调彼得森电流在加热离子被“磁化”（即，回旋频率和碰撞时间的乘积是一阶的）。 第二个模型将处理一维空间中随时间变化的激波形成及其对加热和超音速射流形成的影响。

Two magnetohydrodynamic models will be developed to study non-thermal heating, the generation of directed plasma flows, and energetic particle acceleration processes in solar and stellar atmospheres. A critical component of both simulations will be a realistic description of transport processes in the form of anisotropic tensors for electric and thermal conductivities, as well as viscosity. Such a treatment is necessary when magnetized plasma is neither in a collisionless, nor collision-dominated regime. One model will describe the propagation of small amplitude waves in two spatial dimensions with special emphasis on the role of Pedersen currents in heating the plasma where ions are "magnetized" (i.e., the product of the cyclotron frequency and the collision time is of order unity). The second model will treat time-dependent shock formation in one spatial dimension and its impact on heating and the formation of supersonic jets.