Origin of planetary nebulae - Morphology, carbon-to-oxygen abundance ratios, and central star multiplicity

Details Origin of planetary nebulae - Morphology, carbon-to-oxygen abundance ratios, and central star multiplicity Origin of planetary nebulae - Morphology, carbon-to-oxygen abundance ratios, and central star multiplicity

Feb 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...301..772z&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 301, Feb. 15, 1986, p. 772-789.

Astronomy and Astrophysics

Astrophysics

212

Abundance, Binary Stars, Planetary Nebulae, Stellar Evolution, Carbon, Main Sequence Stars, Oxygen, Ratios, Red Giant Stars, Stellar Magnitude, Stellar Mass Ejection

Scientific paper

The authors have examined data pertaining to the morphology, carbon-to-oxygen abundance ratio, and central star multiplicity of 139 planetary nebulae (PNs). Among 108 nonstellar PNs, ≡50% display a bipolar symmetry, and an additional ≡30% display elliptical symmetry. Comparison of the sizes of extreme red giant stars and separations of main-sequence, solar-type binary stars suggests that the gravitational field of a companion star is unlikely to be responsible for the mass ejection in all or even a majority of these cases. However, it is perhaps conceivable that a secondary star is responsible for most of the above-mentioned symmetries. Based on optical, ultraviolet, infrared, and radio data, the authors find 42 C-rich and 26 O-rich PNs in the set. These numbers agree with the relative numbers of C- and O-rich red giant stars with large mass loss rates and are consistent with the idea that the progenitors of PNs are this class of red giant stars.

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