⢠Spectral line broadening i t h i l l i t h i l l in astrophysical plasmas
⢠Spectral line broadening i t h i l l i t h i l l in astrophysical plasmas
⢠Spectral line broadening i t h i l l i t h i l l in astrophysical plasmas
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• Classical value for the natural <strong>l<strong>in</strong>e</strong> width(Full Width at Half Intensity Maximum –FWHM) does not depend on atomiccharacteristics and plasma conditions and• is equal to 0.000118 Å. The <strong>l<strong>in</strong>e</strong> profile isthe Lorentz one.