Conditions for Photospherically Driven Alfvenic Oscillations to Heat the Solar Chromosphere by Pedersen Current Dissipation

摘要: A magnetohydrodynamic model that includes a complete electrical conductivity tensor is used to estimate conditions for photospherically driven, linear, non-plane Alfvenic oscillations extending from the photosphere lower corona drive chromospheric heating rate due Pedersen current dissipation comparable net radiative loss of $\sim 10^7$ ergs-cm$^{-2}$-sec$^{-1}$. The rates electron in and are also computed. wave amplitudes computed self-consistently as functions an inhomogeneous background (BG) atmosphere. effects resolved numerically using resolution 3.33 m. flux $F_{Ch} \sim 10^7 - 10^8$ ergs-cm$^{-2}$-sec$^{-1}$ at frequencies $\nu 10^2 10^3$ mHz BG magnetic field strengths $B \gtrsim 700$ G perturbation 0.01 0.1$ $B$. total resistive increases with $\nu$. Most occurs photosphere. Thermalization Poynting regulates into chromosphere, limiting $F_{Ch}$. $F_{Ch}$ initially $\nu$, reaches maximum, then decreases increasing $\nu$ needed resolve 10$ m km upper proportional $\nu^{-1/2}$. Estimates suggest these normal modes photospheric tubes diameters 10-20$ km, excited by reconnection sheets thicknesses km.