  In this work, we simulate the evolution of the solar wind along its main
sequence lifetime and compute its thermal radio emission. To study the
evolution of the solar wind, we use a sample of solar mass stars at different
ages. All these stars have observationally-reconstructed magnetic maps, which
are incorporated in our 3D magnetohydrodynamic simulations of their winds. We
show that angular-momentum loss and mass-loss rates decrease steadily on
evolutionary timescales, although they can vary in a magnetic cycle timescale.
Stellar winds are known to emit radiation in the form of thermal bremsstrahlung
in the radio spectrum. To calculate the expected radio fluxes from these winds,
we solve the radiative transfer equation numerically from first principles. We
compute continuum spectra across the frequency range 100 MHz - 100 GHz and find
maximum radio flux densities ranging from 0.05 - 8.3 $\mu$Jy. At a frequency of
1 GHz and a normalised distance of d = 10 pc, the radio flux density follows
0.24 $(\Omega/\Omega_{\odot})^{0.9}$ (d/[10pc])$^2$ $\mu$Jy, where $\Omega$ is
the rotation rate. This means that the best candidates for stellar wind
observations in the radio regime are faster rotators within distances of 10 pc,
such as $\kappa^1$ Ceti (2.83 $\mu$Jy) and $\chi^1$ Ori (8.3 $\mu$Jy). These
flux predictions provide a guide to observing solar-type stars across the
frequency range 0.1 - 100 GHz in the future using the next generation of radio
telescopes, such as ngVLA and SKA.
