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In a more formal definition, the L shell is initially fully occupied. In this case, the lighter species with K-alpha is neon. [5] This choice also places K-alpha firmly in the X-ray energy range. Similarly to Lyman-alpha, the K-alpha emission is composed of two spectral lines, K-alpha 1 (Kα 1) and K-alpha 2 (Kα 2). [6]
A spectral line may be observed either as an emission line or an absorption line. Which type of line is observed depends on the type of material and its temperature relative to another emission source. An absorption line is produced when photons from a hot, broad spectrum source pass through a cooler material.
The K-line is a spectral peak in astronomical spectrometry used, along with the L-line, to observe and describe the light spectrum of stars. The K-line is associated with iron (Fe) and is described as being from emissions at ~6.4keV (thousands of electron volts ).
K-line in spectrometry refers to one of two different spectral features: The calcium K line, one of the pair of Fraunhofer lines in the violet associated with ionised calcium The x-ray peak ( K-line (x-ray) ) associated with iron
Following Bohr's lead, Moseley found that for the spectral lines, this relationship could be approximated by a simple formula, later called Moseley's Law. [2] = where: is the frequency of the observed X-ray emission line
Zeeman effect on a sunspot spectral line George Ellery Hale was the first to notice the Zeeman effect in the solar spectra, indicating the existence of strong magnetic fields in sunspots. Such fields can be quite high, on the order of 0.1 tesla or higher.
In physics, one thinks of a spectral line from two viewpoints. An emission line is formed when an atom or molecule makes a transition from a particular discrete energy level E 2 of an atom, to a lower energy level E 1, emitting a photon of a particular energy and wavelength. A spectrum of many such photons will show an emission spike at the ...
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 ]