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), H-gamma (blue-violet, at 434.0 nm), and H-delta (violet, at 410.2 nm). These lines are important in spectroscopy because they are easily visible through optical instruments and serve as key indicators of the physical conditions in stars and gaseous nebulae.

In stellar astronomy, the strength and shape of Balmer lines are used to determine stellar temperature and gravity. They are especially prominent in the spectra of A-type stars, which exhibit strong Balmer absorption lines due to their specific temperature range. Additionally, the Balmer lines play a significant role in the study of emission nebulae and active galactic nuclei, where they often appear in emission rather than absorption.

The discovery and analysis of Balmer lines have provided critical insights into atomic physics, quantum mechanics, and the structure of stellar atmospheres. Their predictable wavelengths also serve as a basis for calibrating spectroscopic instruments and measuring redshifts in extragalactic objects. Overall, the Balmer series remains a fundamental component in the field of astrophysics and spectroscopy.

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