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Balmer series

(hydrogen lines for electrons settling from n > 2 to n = 2)

The Balmer series is a set of hydrogen spectral lines emitted when the electron orbit descends from n greater than 2 to n = 2. The series is named for Johann Balmer. (As opposed to the Lyman series, from n greater than 1 to n = 1.)

wavelength = Balmer's constant × ( m² / ( m²-n² )

Balmer's constant = 3.6450682 × 10-7 m or 364.50682 nm (same as 4/RH, the Rydberg constant for Hydrogen).

The Balmer series, especially H-α is used to determine the redshift of quasars and distant galaxies because it is often prominent.


(Balmer,hydrogen,line series,lines,spectrum)
http://en.wikipedia.org/wiki/Balmer_series
WaveLFreqPhoton
Energy
  
364nm824THz3.5eVbeginBalmer series
656nm457THz1.9eVendBalmer series

Referenced by:
Balmer jump
Balmer-break galaxy (BBG)
Be star
Bohr model
Brackett series
emission line galaxy (ELG)
H-alpha (Ha)
HII region (HII)
hydrogen (H)
hyperfine structure
Lyman series
Paschen series
quasar (QSO)
star formation rate (SFR)
spectral line energy distribution (SLED)
spectral line

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