  We perform broadband ($0.7-100$ keV) spectral analysis of five hard state
observations of the low-mass back hole X-ray binary GX~339--4 taken by AstroSat
during the rising phase of three outbursts from $2019$ to $2022$. We find that
the outburst in 2021 was the only successful/full outburst, while the source
was unable to make transition to the soft state during the other two outbursts
in 2019 and 2022. Our spectral analysis employs two different model
combinations, requiring two separate Comptonizing regions and their associated
reflection components, and soft X-ray excess emission. The harder Comptonizing
component dominates the overall bolometric luminosity, while the softer one
remains relatively weak. Our spectral fits indicate that the disk evolves with
the source luminosity, where the inner disk radius decreases with increasing
luminosity. However, the disk remains substantially truncated throughout all
the observations at the source luminosity of $\sim2-8\%\times$ of the Eddington
luminosity. We note that our assumption of the soft X-ray excess emission as
disk blackbody may not be realistic, and this kind of soft excess may arise due
the non-homogeneity in the disk/corona geometry. Our temporal analysis deriving
the power density spectra suggests that the break frequency increases with the
source luminosity. Furthermore, our analysis demonstrates a consistency between
the inner disk radii estimated from break frequency of the power density
spectra and those obtained from the reflection modelling, supporting the
truncated disk geometry in the hard state.
