On the helium abundance and physical conditions in the 30 Doradus Nebula

Details On the helium abundance and physical conditions in the 30 Doradus Nebula On the helium abundance and physical conditions in the 30 Doradus Nebula

Oct 1974

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1974a%26a....35..417h&link_type=abstract

Astronomy and Astrophysics, vol. 35, no. 3, Oct. 1974, p. 417-420.

Astronomy and Astrophysics

Astrophysics

12

Abundance, H Alpha Line, Helium, Magellanic Clouds, Nebulae, H Ii Regions, Hydrogen Ions, Ionized Gases, O Stars, Radiant Flux Density, Radiative Recombination

Scientific paper

An ionized helium abundance of 5-8% by number relative to hydrogen is derived from observations of H 109 alpha and He 109 alpha line intensities in 30 Doradus. The value supports the idea that the same mechanism responsible for helium formation in our Galaxy is operative in other galaxies. The lines are about twice as broad as those from typical galactic H II regions and show no indication of blended multiple line components. Nonthermal equilibrium effects are less than 5% in the low density gas of the nebula. Either the stellar luminosity function is different or the ionizing O-star cluster is much more massive in 30 Doradus than in our Galaxy.

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