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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 format and program structure
1994A CNC program is a set of instructions that is read by the machine tool computer system to control machine slide movements, tool movements and additional miscellaneous functions. There are two types of CNC programming: conversational format and word address format.
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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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Center-to-limb variation of solar line profiles as a test of NLTE line formation calculations
Astronomy and Astrophysics, 2004CARLOS Allende Prieto, M Asplund
exaly
On the Formation of Squall Lines
Bulletin of the American Meteorological Society, 1952openaire +1 more source
[O ii] as a proxy for star formation in AGN host galaxies: beware of extended emission line regions
Monthly Notices of the Royal Astronomical Society, 2018Natasha Maddox, Maddox Natasha
exaly