Making the corona and the fast solar wind: a self-consistent simulation for the low-frequency Alfvén waves from photosphere to 0.3AU

We show that the coronal heating and the fast solar wind acceleration in the coronal holes are natural consequence of the footpoint fluctuations of the magnetic fields at the photosphere, by performing one-dimensional magnetohydrodynamical simulation with radiative cooling and thermal conduction. We initially set up a static open flux tube with temperature 10K rooted at the photosphere. We impose transverse photospheric motions corresponding to the granulations with velocity 〈dv⊥〉 = 0.7km/s and period between 20 seconds and 30 minutes, which generate outgoing Alfvén waves. We self-consistently treat these waves and the plasma heating. After attenuation in the chromosphere by ≃ 85% of the initial energy flux, the outgoing Alfvén waves enter the corona and contribute to the heating and acceleration of the plasma mainly by the nonlinear generation of the compressive waves and shocks. Our result clearly shows that the initial cool and static atmosphere is naturally heated up to 10K and accelerated to ≃ 800km/s. (The mpeg movie for fig.1 is available at http://www-tap.scphys.kyoto-u.ac.jp/~stakeru/research/suzuki_200506.mpg Subject headings: magnetic fields – plasma – magnetohydrodynamics – Sun : corona – solar wind – waves