  By using our previous results of magnetohydrodynamical simulations for the
solar wind from open flux tubes, I discuss how the solar wind in the past is
different from the current solar wind. The simulations are performed in fixed
one-dimensional super-radially open magnetic flux tubes by inputing various
types of fluctuations from the photosphere, which automatically determines
solar wind properties in a forward manner. The three important parameters which
determine physical properties of the solar wind are surface fluctuation,
magnetic field strengths, and the configuration of magnetic flux tubes.
Adjusting these parameters to the sun at earlier times in a qualitative sense,
I infer that the quasi-steady-state component of the solar wind in the past was
denser and slightly slower if the effect of the magneto-centrifugal force is
not significant. I also discuss effects of magneto-centrifugal force and roles
of coronal mass ejections.
