Abstract : Stellar bars are ubiquitous in disc galaxies (including the Milky Way) in the Local Universe, with about two-thirds of them harbouring a stellar bar. Bars are present in high redshift (z ~1) disc galaxies as well. Recent JWST observations further revealed the presence of conspicuous stellar bars even at a higher redshift (z ~ 3). At these high redshifts, the galactic discs are known to be thick, kinematically hot (and turbulent), and more gas rich. A consensus of whether these bars are tidally-induced or formed due to the internal gravitational instability is still largely missing. In this talk, I will present results regarding the bar formation scenario in the presence of (kinematically-hot) thick discs using a suite of N-body models of (kinematically cold) thin and (kinematically hot) thick discs. I will further discuss the physical processes involved behind different bar formation scenarios as well as how the thick disc mass fraction impacts the properties and morphology of the resulting stellar bar. In addition, I will briefly mention the robustness of different bar instability criteria when applied to this suite of simulated barred galaxies.