Balmer lines

Definition

Balmer lines are a series of spectral line emissions of hydrogen that occur when an electron transitions from a higher energy level (n > 2) to the n=2 energy level. They are prominent in astronomical spectroscopy and are used to identify and analyze stars' compositions and properties.

5 Must Know Facts For Your Next Test

1. The Balmer series includes visible wavelengths, which is why these lines are often observed in the spectra of stars.
2. The most commonly seen Balmer lines include H-alpha (656 nm), H-beta (486 nm), H-gamma (434 nm), and H-delta (410 nm).
3. Balmer lines are named after Johann Balmer, who first derived their mathematical formula in 1885.
4. These lines are crucial for determining the temperature and composition of stellar atmospheres.
5. In hotter stars, Balmer lines appear stronger because hydrogen atoms are more likely to be ionized at high temperatures.

Review Questions

• What transition do electrons make to produce Balmer lines?
• Why are Balmer lines important for analyzing starlight?
• Which scientist is credited with deriving the mathematical formula for the Balmer series?

Related terms

Spectral Lines: Dark or bright lines that appear in a spectrum due to absorption or emission of light at specific wavelengths by elements.

Stellar Spectroscopy: The study of the spectral properties of stars to understand their composition, temperature, density, mass, distance, luminosity, and relative motion.

Lyman Series: A series of spectral line emissions for hydrogen that occur when an electron transitions from a higher energy level to the n=1 energy level; primarily in ultraviolet range.