Young stars assemble their mass by accreting from the circumstellar disk, leading to the co-evolution of the disk, the birth bed of planets. However, the process of accretion is not steady. It varies by a factor of few to hundreds on timescales ranging from days to centuries. The excess luminosity during the higher order variabilities, also called outbursts, have lasting consequences on the thermal, chemical, and mineralogical history of the disk. Moreover, what physical mechanism triggers these outbursts remains elusive, partly due to a smaller sample of observed outbursts, but largely owing to dissimilar evolutionary profiles.  It underscores the careful study of each and every outbursting young star. In this talk, I will outline the results from the latest outburst of Gaia24ccy, a young stellar object. Utilising the observational signatures of similarity, timescales, mass reservoirs, and disk heating, we could constrain that the outburst was possibly triggered by a thermal instability due to inhomogeneous accretion in the disk at around ~0.047 au.