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
- The Balmer series includes visible wavelengths, which is why these lines are often observed in the spectra of stars.
- The most commonly seen Balmer lines include H-alpha (656 nm), H-beta (486 nm), H-gamma (434 nm), and H-delta (410 nm).
- Balmer lines are named after Johann Balmer, who first derived their mathematical formula in 1885.
- These lines are crucial for determining the temperature and composition of stellar atmospheres.
- 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?
"Balmer lines" appears in:
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.
