Supernovae (SNe) are the cosmic fireworks marking the death of stars, wherein heavy elements are forged and dispersed, leading to the galactic enrichment of the Universe. In core-collapse supernovae (CCSNe), the collapse of the inert Fe core in massive stars, paves the way for the catastrophic explosion. This gives rise to a range of observational signatures owing to the diverse nature of the pre-explosion star and its environment. Hence, decoding the properties of the progenitor and its immediate environment calls for a comprehensive study of these events. In this thesis, we characterized six hydrogen-rich CCSNe (SNe 2014cx, 2014cy, 2015an, 2015ba, AT2015cz, 2016B), arising from progenitors which have managed to retain most of its hydrogen envelope prior to explosion, by photometric and spectroscopic monitoring of these events from Indian and international telescopes. We performed analysis and modelling of the data to constrain progenitor properties and explosion parameters. We ascertained from spectral modelling that circumstellar interaction is prevalent in all SNe II to some extent, which gets subdued in most cases because of their high expansion velocities. Moreover, we determined distances to three host galaxies using the expanding photosphere method (EPM), which unlike some other standard candle methods, is independent of external calibration. The conundrum surrounding the progenitor mass of SNe II from direct imaging has also been explored in this thesis for the case of SN 2015ba, for which we estimated a progenitor mass of around 24-26 Msun, higher than the upper limit proposed from pre-explosion images (18 Msun).