Unveiling U Gem Outbursts: Light Curve Analysis and Exploring Correlations of Outburst Mechanism

As a nova-typed cataclysmic star, U Gem exhibits outbursts in brightness, and stars like this have left astronomers puzzled about the underlying mechanism. By analyzing the light curve of U Gem (a graph representing its changing magnitude over time that reveals the outburst cycle), the spectrums and the temperature variation of its white dwarf component, we gained a bit of understanding of these outbursts. Using professional data sites such as the American Association of Variable Star Observers (AAVSO) and the Cosmic Origins Spectrograph (COS) on the Hubble Space Telescope (HST), we gathered light curves to identify different phases of outbursts as well as collected the visible and ultraviolet spectrums. During the narrow and wide outbursts, it brightens about an average of 4.7 mags, and 5.6667 mags, respectively, in Vis. band, the radial velocity increased 314.486 ± 11.2 km/s throughout different phases, and the WD cools from a temperature of ~41,500 K, 15 days after the peak of the outburst, to ~36,250 K, 56 days after the peak of the outburst. By studying periods of outbursts, we have linked them to material activities in U Gem. To follow the variations in radial velocity during outburst phases, the Balmer spectral lines were also investigated. Correlating these phases with variations in radial velocity, derived from spectral line shifts, and white dwarf temperature changes during quiescence provides crucial insights into the system's behavior and helps to understand the dynamics of the accretion disk and the evolution of cataclysmic variable stars. This, I hope, will make it easier for others who may wish to study further about cataclysmic variable stars and the intricate dynamics of peculiar stars like this one to do so.