BalmerLinien
Balmerlinien, also known as Balmer lines, refer to a specific series of spectral lines in the visible spectrum of hydrogen. These lines are observed when an electron in a hydrogen atom transitions from a higher energy level (n ≥ 3) down to the second energy level (n=2). They are named after Johann Balmer, who formulated an empirical equation describing their wavelengths in 1885.
The Balmer series includes four prominent lines: H-alpha (red, at 656.3 nm), H-beta (blue-green, at 486.1 nm),
In stellar astronomy, the strength and shape of Balmer lines are used to determine stellar temperature and
The discovery and analysis of Balmer lines have provided critical insights into atomic physics, quantum mechanics,
---