Hydrogen recombination lines - A model of the temperature and density in Orion A

Details Hydrogen recombination lines - A model of the temperature and density in Orion A Hydrogen recombination lines - A model of the temperature and density in Orion A

Oct 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...184..291w&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 184, no. 1-2, Oct. 1987, p. 291-299.

Astronomy and Astrophysics

Astrophysics

25

Abundance, H Alpha Line, H Beta Line, Orion Nebula, Bandwidth, Electron Density (Concentration), Electron Energy, Parameterization, Spectral Line Width

Scientific paper

Five point maps in the H 110-alpha and H 139-beta lines are used to model Orion A. At 4 min from the continuum peak, the radio recombination lines are shown to form in LTE. The present model indicates that Orion A consists of nine face-on cylindrical slabs placed on axis, and that the densest part of the nebula is hotter (an electron temperature of 8500 K) than the surrounding lower density gas. Electron density features follow the model of Shaver (1980), with ionized gas in all regions of Orion A being clumped, and with volume filling factors of about 0/1 being necessary in order to obtain consistency with the radio recombination line data.

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