Statistics – Computation
Scientific paper
Apr 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991ap%26ss.178...45e&link_type=abstract
Astrophysics and Space Science (ISSN 0004-640X), vol. 178, no. 1, April 1991, p. 45-69.
Statistics
Computation
Helium Atoms, Stellar Atmospheres, Boltzmann Distribution, Computational Astrophysics, Neutral Atoms
Scientific paper
The deviations from the Boltzmann distribution are calculated for over 93 energy levels of neutral He atoms and for quantum numbers of up to n = 10. The dilution factor and the electron temperature are the key parameters for the equations which are based on previous computations and extended to higher levels including visible and photographic He I emission lines. The cases where electron temperature (TE) and radiation temperature (TS) have different values allow applications of the results to cases such as lower and intermediate atmospheres. The results of the calculations are listed, and the discrepancies with previous calculations can be explained by the fact that the calculations presented consider more energy levels. All b-factors are greater than or equal to unity when TE is less than or equal to TS, and the ground and metastable levels of cases where TE = TS do not change when highly dilute.
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