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

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Spectral type and effectivetemperature of a star can bedetermined by comparing itsspectrum with a standard spectrumfor a spectral type and effectivetemperature. In Fig. left are spectraltypes and right effectivetemperatures.
PRESSURE BROADENING• VAN DER WAALS BROADENING – broadening bycollisions with neutral atoms• RESONANCE BROADENING – broadening due tonon radiative charge exchange for atoms of thesame kind when one of the energy levels l of thetransition responsible for the line has an allowedtransition on the ground level• STARK BROADENING – broadening by interactionwith charged particles producing Stark effect –splitting and shift of atomic energy levels dependingon the strength of electric field.
Page 1 and 2: • Spectral line broadeningin astr
Page 3: EMISSION SPECTRAL LINEWith I is den
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