We analyze the results of photometric monitoring of comet C/2013 X1 (PANSTARRS) from December 2015 until January 2016 obtained within B V and R Johnson-Cousins filters. The main objective is to investigate the dust coma and to obtain the physical characteristics of its dust particles. We analyzed our observations using model-agglomerated debris particles, and we constrained the microphysical properties of the dust in comet C/2013 X1 (PANSTARRS) on the pre-outburst and post-outburst epochs. Moreover, we applied a geometrical model to the images processed by digital filters to estimate the rotational period of the nucleus. Our campaign revealed a sharp increase in the comet brightness on January 1, 2016. The $B-V$ and $V-R$ colors calculated within an aperture size of 17\,000 km appear to be mostly red, except for the outburst date. The dust production ($Af proxy) and normalized spectral gradient prime (B-R)$ dramatically changed on January 2 as compared to what was seen in December 2015. According to this model, the C/2013 X1 coma was populated by 70<!PCT!> organic-matter particles by volume and by two types of silicate particles together, constituting the other 30<!PCT!>. One type of silicate particles was composed of Mg-rich silicates, whereas the other type was composed of both Mg-rich and Fe-poor silicates. Using the geometrical model, we estimate the nucleus rotational period to be ($24.02 0.02$) h. We interpret the observed coma morphology by two jet structures, one structure that formed by the near-pole active area at a latitude of circ $, and the other structure formed by an active area at a latitude of $(+40 circ