The Necessity of Using Realistic Descriptions of Transport Processes in Modeling the Solar Atmosphere, and the Importance of Understanding Chromospheric Heating*

摘要: Three points and research directions are discussed: The outstanding problem of identifying the mechanisms solar atmospheric heating wind acceleration can be solved only by combining quantitative models that include realistic descriptions relevant transport processes with observational constraints on inputs outputs these models. Most heating, possible exception flares, takes place in chromosphere, emphasizing importance chromospheric which may important for understanding coronal acceleration. Recent modeling leads to conclusion onset proton magnetization increasing height thin magnetic flux tubes triggers network resistive dissipation Pedersen currents driven convection electric field slow, longitudinal magnetoacoustic waves.