â¢ Spectral line broadening i t h i l l i t h i l l in astrophysical plasmas

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• THE BASIC ARTICLES ON MODIFIEDSEMIEMPIRICAL APPROACH ARE IN THEFOLDER BIBLIOGRAPHY_DIMITRIJEVIC:• 1. Dimitrijević, M. S., Konjević, N., 1981, SpectralLine Shapes 1, Walter de Gruyter, p. 211.• 2. Dimitrijević, M. S., Kršljanin, V., 1986, A&A, 165,269.• 3. Dimitrijević, M.S., Popović, L. Č., 2001, Journal ofApplied Spectroscopy, 68, 893
SYMPLIFIED MODIFIEDSEMIEMPIRICAL FORMULA•For the astrophysical purposes, of particular interest•might be the symplified semiempirical formula for•Stark widths of isolated, singly, and multiply l chargedion lines applicable in the cases when the nearestatomic energy level (j'=i‘ or f') f)where a dipollyallowed transition can occur from or to initial (i) orfinal (f) energy level of the considered line, is sofar, that the condition x jj΄= E/( E j΄ -E j ) smaller thanor equal to 2 is satisfied.In such a cases full width at half maximum isgiven by the expression:
Page 1 and 2: • Spectral line broadeningin astr
Page 3 and 4: EMISSION SPECTRAL LINEWith I is den
Page 5 and 6: PRESSURE BROADENING• VAN DER WAAL
Page 7 and 8: NATURAL BROADENING• Natural broad
Page 9: LORENTZ PROFILEI - Intensity; γ =W
Page 12 and 13: •
Page 14 and 15: Here v barr is the average relative
Page 16 and 17: • an excited atom and an atom in
Page 19 and 20: NEEDS FOR LARGE STARKBROADENING DAT
Page 21 and 22: • STARK BROADENING IS IMPORTANTFO
Page 23 and 24: INTERSTELLAR MOLECULARCLOUDS• In
Page 26 and 27: • For example, the influence of S
Page 28: • Line shapes enter in the models
Page 32 and 33: • THERE IS MORE INFORMATION IN TH
Page 34: • This is, among other reasons, t
Page 44 and 45: STARK BROADENING• SEMICLASSICAL M
Page 46 and 47: • The literature and some nummeri
Page 48 and 49: • Due to the considerably smaller
Page 53: •Here, N and T are the electron d
Page 57 and 58: • THE BASIC ARTICLE ON THE SYMPLI
Page 59 and 60: STARK-B• http://stark-b.obspm.fr/
Page 61 and 62: SPECTRAL LINE SHAPES INYUGOSLAVIA A

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â¢ Spectral line broadening i t h i l l i t h i l l in astrophysical plasmas