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Line Formation in Turbulent Media
1975Since 1934, when Struve and Elvey introduced the concept of microturbulence for spectral line broadening in addition to pressure and thermal Doppler broadening, this mechanism has frequently been used in the analysis of stellar spectra. According to the discussions in standard textbooks on stellar spectra the effect of microturbulence is due to an ...
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Formation of FEII Lines in AGN
1988Up to now photoionization models of the Broad Line Region of quasars fail to explain the strength of low ionization lines, in particular, FeII lines are too weak compared to H3. Using a code mainly designed to study low ionized and optically thick medium, I have calculated the radiation transfer in a non-photoionized homogeneous cloud in order to ...
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Line formation in solar granulation
Astronomy and Astrophysics, 2004Martin Asplund, A J Sauval, N Grevesse
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Non-LTE formation of the Fe I 6173 Å line in the solar atmosphere
Astronomy and Astrophysics, 2023Sami Solanki, H N Smitha, M van Noort
exaly
On the Formation of Squall Lines
Bulletin of the American Meteorological Society, 1952openaire +1 more source
Center-to-limb variation of solar line profiles as a test of NLTE line formation calculations
Astronomy and Astrophysics, 2004Martin Asplund, C Allende Prieto
exaly
Effects of line-blocking on the non-LTE Fe I spectral line formation
Astronomy and Astrophysics, 2005Remo Collet, Martin Asplund
exaly