  The solar wind (SW) is a supersonic outflow of plasma from the solar corona,
with the latitudinal speed and density profiles varying with the solar
activity. The SW protons charge exchange with the inflowing interstellar
neutral atoms and create energetic neutral atoms (ENAs), which bring
information on the physical state of the plasma within the boundary region of
the heliosphere. The speed of the ENAs depends on their energies, and
consequently observations at different energies provide information on
different epochs backwards in time. Therefore, understanding the history of the
evolution of the SW is important to understand this information. In this paper,
we extend the work by \citet{porowski_etal:22a}, who provided the WawHelioIon
3DSW model of the time evolution of latitudinal profiles of the SW speed and
density based on results of analysis of interplanetary scintillations (IPS).
Based on results of Principal Component Analysis, we seek for correlation
between selected solar proxies and the structure of the SW obtained from IPS
and show that it is possible to reproduce the evolution of the SW structure
during the past three solar cycles based on the proxies. With this, we extend
the history of the evolution of the SW structure back to 1976, i.e., to the
epoch when observations of the key proxies -- the inclination of the SW current
sheet and the solar polar magnetic fields -- became available. We point out the
potential of the use of the proxies for forecasting the structure of the SW
into the future.
