Self-consistent MHD modeling of solar wind acceleration
Suzuki, T. K. and Inutsuka, S.
We show that the coronal heating and the 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 impose transverse photospheric motions corresponding to the granulations
with velocity 0.7km/s and period between
20 seconds and 30 minutes, which generate outgoing Alfven waves.
After attenuation in the chromosphere by ~85% of the initial
energy flux, the outgoing Alfven waves enter the corona and contribute
to the heating and acceleration of the plasma mainly through nonlinear
generation of the compressive waves.
Finally, we discuss relations between the photospheric magnetic fields and
the above coronal properties predicted from our simulations, which can be
directly tested by observations of various coronal holes by Solar-B.
Correspondence
Takeru Suzuki (stakeru@scphys.kyoto-u.ac.jp), Kyoto University
presentation
invited