Astrophysics (Index)About

Balmer series

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

The Balmer series is the set of hydrogen spectral lines emitted when an electron descends from an electron shell number n greater than 2 down to n = 2, or the analogous absorption lines when absorbed electromagnetic radiation makes the electron do the opposite. It is one of the hydrogen line series, such as the Lyman series and is named after Johann Balmer. Lines:

Formula for the wavelengths:

wavelength = Balmer's constant × n² / ( n²-4 )

where

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)
Further reading:
http://en.wikipedia.org/wiki/Balmer_series
WaveLFreqPhoton
Energy
  
364nm824THz3.5eVbeginBalmer series
656nm457THz1.9eVendBalmer series

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

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