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Coronal mass ejections (CMEs) and high speed solar streams serve asperturbations to the background solar wind that have major implications inspace weather dynamics. Therefore, a robust framework for accurate predictionsof the background wind properties is a fundamental step towards the developmentof any space weather prediction toolbox. In this pilot study, we focus on theimplementation and comparison of various models that are critical for a steadystate, solar wind forecasting framework. Specifically, we perform case studieson Carrington rotations 2053, 2082 and 2104, and compare the performance ofmagnetic field extrapolation models in conjunction with velocity empiricalformulations to predict solar wind properties at Lagrangian point L1. Twodifferent models to extrapolate the solar wind from the coronal domain to theinner-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 hydrodynamicsusing the PLUTO code and can additionally predict the thermal properties ofsolar wind. The assessment in predicting solar wind parameters of the differentmodels is quantified through statistical measures. We further extend thisdeveloped framework to also assess the polarity of inter-planetary magneticfield at L1. Our best models for the case of CR2053 gives a very highcorrelation 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 standarddeviation comparable with that obtained from the hourly OMNI solar wind dataand also produces a considerable match with observed solar wind protontemperatures measured at L1 from the same database.

A comparison study of extrapolation models and empirical relations in forecasting solar wind