  In the present paper, we model the wind of solar analogues at different ages
to investigate the evolution of the solar wind. Recently, it has been suggested
that winds of solar type stars might undergo a change in properties at old
ages, whereby stars older than the Sun would be less efficient in carrying away
angular momentum than what was traditionally believed. Adding to this, recent
observations suggest that old solar-type stars show a break in coronal
properties, with a steeper decay in X-ray luminosities and temperatures at
older ages. We use these X-ray observations to constrain the thermal
acceleration of winds of solar analogues. Our sample is based on the stars from
the `Sun in time' project with ages between 120-7000 Myr. The break in X-ray
properties leads to a break in wind mass-loss rates ($\dot{M}$) at roughly 2
Gyr, with $\dot{M}$ (t < 2 Gyr) $\propto t^{-0.74}$ and $\dot{M}$ (t > 2 Gyr)
$\propto$ $t^{-3.9}$. This steep decay in $\dot{M}$ at older ages could be the
reason why older stars are less efficient at carrying away angular momentum,
which would explain the anomalously rapid rotation observed in older stars. We
also show that none of the stars in our sample would have winds dense enough to
produce thermal emission above 1-2 GHz, explaining why their radio emissions
have not yet been detected. Combining our models with dynamo evolution models
for the magnetic field of the Earth we find that, at early ages ($\approx$100
Myr) our Earth had a magnetosphere that was 3 or more times smaller than its
current size.
