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

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•Here, N and T are the electron density andtemperature respectively, E = 3kT/2 is the energy ofperturbing electron, Z-1 is the ionic charge and n theeffective principal quantum number. This expression isof interest for abundance calculations, as well as forstellar atmospherae research, since the validityconditions are often satysfied for stellar plasmaconditions.• Similarly, in the case of the shift:
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 50 and 51: • THE BASIC ARTICLES ON MODIFIEDS
Page 55: • If all levels l i,f ±1 exist,
Page 58 and 59: SOME USEFUL DATABASES• ATOMIC ENE
Page 60 and 61: • The impact approximation i and
Page 62: THANK YOUFORATTENTION

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