Astrophysics (index)

Balmer Series

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

The Balmer Series is a set of Hydrogen (H) 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.)

  • 3 -> 2: H-alpha (Ha), H-α. 656.3 nm (red)
  • 4 -> 2: H-beta, H-β 486.1 nm (cyan)
  • 5 -> 2: H-gamma, H-γ 434.1 nm (blue)
  • 6 -> 2: H-delta, H-δ 410.2 nm (violet)
  • 7 -> 2: H-epsilon, H-ε 397.0 nm (Ultraviolet (UV))
  • 8 -> 2: H-zeta, H-ζ 388.9 nm (ultraviolet)
  • 9 -> 2: H-eta, H-η 383.5 nm (ultraviolet)
  • infinity -> 2: 364.6 nm (ultraviolet)

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 (z) of Quasars (QSO) and distant galaxies because it is often prominent.


(Balmer,hydrogen,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

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