Star formation and its consequential effects play a major role in the physical and chemical evolution of a galaxy and its energetic. We studied a sample of Wolf-Rayet (WR) galaxies to understand some of these effects related to massive start formation in galaxies. The galaxy-galaxy tidal interaction or merger is expected to be primary mechanism for star-burst in galaxies. We performed Hα line imaging using 1.3-m DFOT to identify interaction/merger features in WR galaxies and also to obtain star formation rates (SFRs). Using the Hα observations and archival data from various sky surveys in FUV, FIR, and radio bands, we constructed various correlations between SFRs estimated using different radiation mechanisms. We also imaged several WR dwarf galaxies in optical spectroscopy using 2-m HCT. We estimated spatially-resolved chemical abundances in different star-forming regions in the WR galaxies. We found that majority of WR dwarf galaxies are chemically homogeneous and the most recent phase of massive star formation not older than 10 Myr or so has not significantly affected the surrounding diffuse interstellar medium. It is likely that supernovae explosions have not yet taken place in WR regions, which is also corroborated by an observed deficiency of the synchrotron radio emission from several WR galaxies. In one case, we found significant metallicity difference between two star forming regions which we could explain in terms of recent merger of two galaxies, with the help of combined optical and GMRT HI 21cm-line images. The spatially resolved abundance studies of WR and dwarf galaxies are rare and are important to understand chemical enrichment histories of dwarf galaxies. We would therefore like to pursue several such galaxies using the 3.6-m DOT and the ADFOSC instrument in up-coming cycles. At present, we are verifying the performance of ADFOSC for such studies.