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The phrase "spectral lines", when not qualified, usually refers to lines having wavelengths in the visible band of the full electromagnetic spectrum. Many spectral lines occur at wavelengths outside this range. At shorter wavelengths, which correspond to higher energies, ultraviolet spectral lines include the Lyman series of hydrogen.
In 1890, Rydberg proposed on a formula describing the relation between the wavelengths in spectral lines of alkali metals. [2]: v1:376 He noticed that lines came in series and he found that he could simplify his calculations using the wavenumber (the number of waves occupying the unit length, equal to 1/λ, the inverse of the wavelength) as his unit of measurement.
Lines of the spectra of elements could be predicted from existing lines. [ 1 ] [ 2 ] Since the frequency of light is proportional to the wavenumber or reciprocal wavelength , the principle can also be expressed in terms of wavenumbers which are the sum or difference of wavenumbers of two other lines.
Therefore, the lines seen in the image above are the wavelengths corresponding to n = 2 on the right, to n → ∞ on the left. There are infinitely many spectral lines, but they become very dense as they approach n → ∞ (the Lyman limit), so only some of the first lines and the last one appear.
Spectral line shape or spectral line profile describes the form of an electromagnetic spectrum in the vicinity of a spectral line – a region of stronger or weaker intensity in the spectrum. Ideal line shapes include Lorentzian , Gaussian and Voigt functions, whose parameters are the line position, maximum height and half-width. [ 1 ]
The spectral lines are grouped into series according to n′. Lines are named sequentially starting from the longest wavelength/lowest frequency of the series, using Greek letters within each series. For example, the 2 → 1 line is called "Lyman-alpha" (Ly-α), while the 7 → 3 line is called "Paschen-delta" (Pa-δ).
Four lines (counting from the right) are formally in the visible range. Lines five and six can be seen with the naked eye, but are considered to be ultraviolet as they have wavelengths less than 400 nm. The Balmer series, or Balmer lines in atomic physics, is one of a set of six named series describing the spectral line emissions of the ...
The theoretical limit for the wavelength in the Pickering-Fowler is given by: =, which is approximatedly 364.556 nm, which is the same limit as in the Balmer series (hydrogen spectral series for =). Notice how the transitions in the Pickering-Fowler series for n=6,8,10 (6560Å ,4859Å and 4339Å respectively), are nearly identical to the ...
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