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In [[atomic physics]], the '''Brackett series''' is a series of [[absorption line|absorption]] or [[emission line]]s that are due to electron transitions between the fourth and higher [[energy level]]s of the [[hydrogen atom]]. These lines lie in the [[infrared]], with [[wavelengths]] from 4.05 micrometres (Brackett-alpha) to 1.46 micrometres (the series limit), and are named after the American physicist [[Frederick Sumner Brackett]] |
In [[atomic physics]], the '''Brackett series''' is a series of [[absorption line|absorption]] or [[emission line]]s that are due to electron transitions between the fourth and higher [[energy level]]s of the [[hydrogen atom]]. These lines lie in the [[infrared]], with [[wavelengths]] from 4.05 micrometres (Brackett-alpha) to 1.46 micrometres (the series limit), and are named after the American physicist [[Frederick Sumner Brackett]] who first observed them in 1922. |
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Brackett series of hydrogen, n=4, in nm: |
Brackett series of hydrogen, n=4, in nm: |
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Revision as of 00:17, 21 July 2006
In atomic physics, the Brackett series is a series of absorption or emission lines that are due to electron transitions between the fourth and higher energy levels of the hydrogen atom. These lines lie in the infrared, with wavelengths from 4.05 micrometres (Brackett-alpha) to 1.46 micrometres (the series limit), and are named after the American physicist Frederick Sumner Brackett who first observed them in 1922.
Brackett series of hydrogen, n=4, in nm:
- 5-4 -- 4052.5
- 6-4 -- 2625.9
- 7-4 -- 2166.1
- 8-4 -- 1945.1
- 9-4 -- 1818.1
limit: 1459 nm
References
- Frederick Sumner Brackett, Visible and Infra-Red Radiation of Hydrogen; Astrophysical Journal, vol. 56, (1922) p.154; DOI: 10.1086/142697
See also
External links
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