The Balmer Series refers to a set of spectral lines that are produced when electrons in a hydrogen atom transition from higher energy levels to the second energy level. These transitions emit light in the visible spectrum, resulting in specific wavelengths that correspond to colors. The Balmer Series is significant in understanding atomic structure and the behavior of electrons. Named after the Swiss mathematician Johann Balmer, who formulated the Balmer formula in 1885, this series includes prominent lines such as H-alpha, H-beta, H-gamma, and H-delta. The Balmer Series is crucial in fields like astronomy and spectroscopy, helping scientists analyze the composition and properties of stars and other celestial bodies.