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

More documents

Recommendations

Info

• an excited atom and an atom in theground state, we can not detect this.However this is an additional possibility forthe shortening of lifetime of the opticalelectron on the considered atomic energylevel so that the corresponding spectralline, in accordance with the Heizenberguncertainty principle, is addiitionallybroadened.
• Ali and Griem (Phys. Rev. A 1966, 140,1044, Phys. Rev. A 144, 366) obtained forthe width of resonantly broadened line infunction of statistical weights g of emitting(e) and absorbing (a) states, density ofatoms of the same kind in the ground stateN and oscillator strength f for the transitionto the ground state, 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 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

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

Create successful ePaper yourself

Delete template?

Save as template?

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