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We present an in-depth spectral and timing analysis of the Black Hole binary4U 1630-472 during 2016 and 2018 outbursts as observed by \textit{AstroSat} and\textit{MAXI}. The extensive coverage of the outbursts with \textit{MAXI} isused to obtain the Hardness Intensity Diagram (HID). The source follows a`c'-shaped profile in agreement with earlier findings. Based on the HIDs ofprevious outbursts, we attempt to track the evolution of the source during a`super'-outburst and `mini'-outbursts. We model the broadband energy spectra($0.7-20.0$ keV) of \textit{AstroSat} observations of both outbursts usingphenomenological and physical models. No Keplerian disc signature is observedat the beginning of 2016 outburst. However, the disc appears within a few hoursafter which it remains prominent with temperature ($T_{in}$) $\sim$ 1.3 keV andincrease in photon index ($\Gamma$) from 1.8 to 2.0, whereas the source was ata disc dominant state throughout the \textit{AstroSat} campaign of 2018outburst. Based on the HIDs and spectral properties, we classify the outburstsinto three different states - the `canonical' hard and soft states along withan intermediate state. Evolution of rms along different states is seen althoughno Quasi-periodic Oscillations (QPOs) are detected. We fit the observed spectrausing a dynamical accretion model and estimate the accretion parameters. Massof the black hole is estimated using inner disc radius, bolometric luminosityand two component flow model to be $3-9$ $M_{\odot}$. Finally, we discuss thepossible implications of our findings.

AstroSat and MAXI view of the Black Hole binary 4U 1630-472 during 2016 and 2018 Outbursts