The forbidden line spectrum in the edges of H II regions

Details The forbidden line spectrum in the edges of H II regions The forbidden line spectrum in the edges of H II regions

May 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977ap%26ss..48..293m&link_type=abstract

Astrophysics and Space Science, vol. 48, no. 2, May 1977, p. 293-296.

Astronomy and Astrophysics

Astrophysics

Forbidden Bands, H Ii Regions, Interstellar Gas, Interstellar Radiation, Line Spectra, Stellar Motions, Forbidden Transitions, Gas Ionization, Gas Mixtures, Hydrogen Ions, Nebulae, Relativistic Effects

Scientific paper

It is shown analytically that the motion of exciting stars can affect the forbidden emission-line spectra of H II regions in an observable manner. A model is used which comprises a small solid angle of a spherical nebula that is symmetric with respect to the direction of stellar motion and consists of a mixture of H, He, C, N, O, and Ne with ionization states up to He II, C III, N III, O III, and Ne III. Consideration is given to the case of a 36-solar-mass O5 star with an effective temperature of 43,000 K moving at a velocity of 10 km/s in a nebula having a density of 10 times the proton mass per cu cm. The results obtained indicate that: (1) the region where forbidden lines characteristic of ionization fronts are produced is broadened considerably at the trailing edge of the nebula; (2) the spectrum in this region is comparable to that of fossil H II regions; and (3) the ionization front at the leading edge is sharper, the temperature there is higher, and the forbidden-line spectrum is similar to that of young ionization fronts.

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