Balmerserie
The Balmer-Serie, or Balmer series, is a hydrogen spectral series corresponding to electronic transitions from higher energy levels to the n = 2 level. Photons emitted by these transitions lie predominantly in the visible part of the spectrum, which is why many hydrogen lines are visible in stars and emission nebulae.
The wavelengths of the Balmer series can be described by the Rydberg formula: 1/λ = R_H (1/2^2 −
The most prominent lines are H-alpha (n = 3 → 2) at 656.3 nm, H-beta (4 → 2) at
Historically, the series is named after Johann Balmer, who in 1885 derived an empirical formula for hydrogen
Significance: In astronomy and spectroscopy, Balmer lines are used to diagnose physical conditions in stars, H