Making the corona and the fast solar wind: A self-consistent simulation for the low-frequency alfven waves from the photosphere to 0.3 Au

By performing a one-dimensional magnetohydrodynamic simulation with radiative cooling and thermal conduction, we show that the coronal heating and the fast solar wind acceleration in the coronal holes are natural consequences of the footpoint fluctuations of the magnetic fields at the photosphere. We initially set up a static open flux tube with a temperature of 104 K rooted at the photosphere. We impose transverse photospheric motions corresponding to the granulations with a velocity < dv(perpendicular to)> = 0.7 km s(-1) and a period between 20 s and 30 minutes, which generate outgoing Alfve ' n waves. We self- consistently treat these waves and the plasma heating. After attenuation in the chromosphere by similar or equal to 85% of the initial energy flux, the outgoing Alfven 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 initially cool and static atmosphere is naturally heated up to 10(6) K and accelerated to similar or equal to 800 km s(-1).