  We use magnetograms of 8 solar analogues of ages 30~Myr to 3.6~Gyr obtained
from Zeeman Doppler Imaging (ZDI) and taken from the literature, together with
two solar magnetograms, to drive magnetohydrodynamical (MHD) wind simulations
and construct an evolutionary scenario of the solar wind environment and its
angular momentum loss rate. With observed magnetograms of the radial field
strength as the only variant in the wind model, we find that power law model
fitted to the derived angular momentum loss rate against time, $t$, results in
a spin down relation $\Omega\propto t^{-0.51}$, for angular speed $\Omega$,
which is remarkably consistent with the well-established Skumanich law
$\Omega\propto t^{-0.5}$. We use the model wind conditions to estimate the
magnetospheric standoff distances for an Earth-like test planet situated at
1~AU for each of the stellar cases, and to obtain trends of minimum and maximum
wind ram pressure and average ram pressure in the solar system through time.
The wind ram pressure declines with time as $\overline{P_{ram}}\propto
t^{2/3}$, amounting to a factor of 50 or so over the present lifetime of the
solar system.
