The solar-type stars shows rich variety of magnetic activities such as surface inhomogeneities due to presence of dark spots, short and long-term variations in spot-cycles and flares. Using the wealth of ∼24 yr multi-band data, we present an in-depth study of the evolution of starspot distributions, optical-flares, Surface Differential Rotations (SDR) and coronal activities on the surface of young, single, main-sequence, Ultra Fast Rotator (UFR) LO Peg. With V-band data a rotational period of 0.422923 ± 0.000005 d has been established. In our study for the first time we have investigated the long-term periods of LO Peg. Evidence of existence of three periods of ∼2.98 yr, ∼7.44 yr and ∼11.8 yr have been detected. Using the seasonal variations on rotational period we also investigate the SDR pattern. LO Peg shows a solar-like pattern of SDR, that is the rotational period steadily decreases along the activity cycle, jumping back to higher values at the beginning of the next cycle with a cycle of 2.8 yr. During the observations 20 optical flares are detected with a derived flare frequency of ∼1 flare per two days. Energies of these flares have been found to vary within a range of 10^{32−34} erg. Using light curve inversion technique (iPH code) we have constructed temperature inhomogeneity map of the surface of LO Peg. The surface coverage of cool spots is found to be in the range of ∼6-27%. It appears that the high and low latitude spots are interchanging their positions. Using XMM-Newton observation, we investigate properties of a flare from the very active and poorly known stellar system 47 Cas. The luminosity at the peak of the flare was found to be 3.54 × 10^30 erg s^{−1} , which is ∼2 times more than that at quiescent state. The quiescent state corona of 47 Cas was represented by two temperature plasma: 3.7 and 11.0 MK. The time-resolved X-ray spectroscopy of the flare showed the variable nature of the temperature, the emission measure, and the abundance. The maximum temperature during the flare was found to be 72.8 MK. We inferred the length of a flaring loop to be 3.3 × 10^10 cm using a hydrodynamic loop model. Using ∼11 years XMM-Newton data we present flare analysis of a young, main-sequence ultra-fast rotator AB Dor. A total of ∼140 X-ray flares were detected in the entire span of observations. Evidence of two temperature quiescent corona at 3.36 MK and 11.1 MK is seen. The density of each flare is derived at the range of 2-10 X 10^10 cm^{−3} . The flaring loop length is found to vary in the order of 1010 cm.