Balmer Series


Balmer Seriessearch for term

A distinct pattern of emission or absorption spectral lines that are caused by the transition of electrons to the n=2 energy level of hydrogen. These spectral lines appear at visible wavelengths, and since stars are mostly composed of hydrogen, the Balmer series of spectral lines is one of the most prominent features in the visible spectrum of a star. The first four Balmer lines of the Balmer series are:

H-alpha: 656.3 nm (red)

H-beta: 486.1 nm (green-blue)

H-gamma: 434.0 nm (blue)

H-delta: 410.1 nm (blue-violet)