  The modeling of the heliosphere requires continuous three-dimensional solar
wind data. The in-situ out-of-ecliptic measurements are very rare, so that
other methods of solar wind detection are needed. We use the remote-sensing
data of the solar wind speed from observations of interplanetary scintillation
(IPS) to reconstruct spatial and temporal structures of the solar wind proton
speed from 1985 to 2013. We developed a method of filling the data gaps in the
IPS observations to obtain continuous and homogeneous solar wind speed records.
We also present a method to retrieve the solar wind density from the solar wind
speed, utilizing the invariance of the solar wind dynamic pressure and energy
flux with latitude. To construct the synoptic maps of the solar wind speed we
use the decomposition into spherical harmonics of each of the Carrington
rotation map. To fill the gaps in time we apply the singular spectrum analysis
to the time series of the coefficients of spherical harmonics. We obtained
helio-latitudinal profiles of the solar wind proton speed and density over
almost three recent solar cycles. The accuracy in the reconstruction is, due to
computational limitations, about 20%. The proposed methods allow us to improve
the spatial and temporal resolution of the model of the solar wind parameters
presented in our previous paper (Sok\'o{\l} et al. 2013) and give a better
insight into the time variations of the solar wind structure. Additionally, the
solar wind density is reconstructed more accurately and it fits better to the
in-situ measurements from Ulysses.
