Determination of nebular density and temperature from radio recombination lines

Details Determination of nebular density and temperature from radio recombination lines Determination of nebular density and temperature from radio recombination lines

Mar 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apjs...57..571o&link_type=abstract

Astrophysical Journal Supplement Series (ISSN 0067-0049), vol. 57, March 1985, p. 571-585. NSF-supported research.

Astronomy and Astrophysics

Astronomy

8

Electron Density (Concentration), Electron Energy, Planetary Nebulae, Radio Astronomy, H Ii Regions, Mass Distribution, Radio Spectra, Weighting Functions

Scientific paper

A method for determining values of nebular electron temperature (Te) and local electron density (ne) is described. The method is based on observations of two well separated H-alpha lines, together with radio continuum observations. Values of Te and ne were derived on the basis of a homogeneous, isothermal model to fit the observations. The weighting of the mean electron density was determined by considering the effects of small-scale density fluctuations. The weighting of the mean electron temperature was carried out using a technique similar to that of Peimbert (1967). The reliability of the method was evaluated by applying it to the calculated emission from various inhomogeneous model nebule with large variations in density along and across the line of sight. It is found that values of Te and ne derived by the new method were in good agreement with actual mean values, even for models with strong stimulated emission. The analysis was also applied to observations of H-II regions and planetary nebulae, and the results were found to agree with results obtained by other methods. A list of the inhomogeneous model nebulae is given.

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