  Coronal mass ejections (CMEs) and high speed solar streams serve as
perturbations to the background solar wind that have major implications in
space weather dynamics. Therefore, a robust framework for accurate predictions
of the background wind properties is a fundamental step towards the development
of any space weather prediction toolbox. In this pilot study, we focus on the
implementation and comparison of various models that are critical for a steady
state, solar wind forecasting framework. Specifically, we perform case studies
on Carrington rotations 2053, 2082 and 2104, and compare the performance of
magnetic field extrapolation models in conjunction with velocity empirical
formulations to predict solar wind properties at Lagrangian point L1. Two
different models to extrapolate the solar wind from the coronal domain to the
inner-heliospheric domain are presented, namely, (a) Kinematics based
(Heliospheric Upwind eXtrapolation [HUX]) model and (b) Physics based model.
The physics based model solves a set of conservative equations of hydrodynamics
using the PLUTO code and can additionally predict the thermal properties of
solar wind. The assessment in predicting solar wind parameters of the different
models is quantified through statistical measures. We further extend this
developed framework to also assess the polarity of inter-planetary magnetic
field at L1. Our best models for the case of CR2053 gives a very high
correlation coefficient ($\sim$ 0.73-0.81) and has an root mean square error of
($\sim$ 75-90 kms$^{-1}$). Additionally, the physics based model has a standard
deviation comparable with that obtained from the hourly OMNI solar wind data
and also produces a considerable match with observed solar wind proton
temperatures measured at L1 from the same database.
