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

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• A spectral line is never monochromatic. Italways has some width due to variousreasons.• BROADENING MECHANISMS:• NATURAL BROADENING• DOPPLER BROADENING – depends onTemperature• PRESSURE BROADENING – depends ontemperature and perturber density(pressure)
EMISSION SPECTRAL LINEWith I is denoted intensity, with c continuum andwith W equivalent width
Page 1: • Spectral line broadeningin astr
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 50 and 51: • THE BASIC ARTICLES ON MODIFIEDS
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

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