Astronomy and Astrophysics – Astrophysics
Scientific paper
Mar 1980
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...236..592k&link_type=abstract
Astrophysical Journal, Part 1, vol. 236, Mar. 1, 1980, p. 592-597.
Astronomy and Astrophysics
Astrophysics
32
Cosmic Dust, Far Infrared Radiation, Planetary Nebulae, Stellar Envelopes, Stellar Evolution, Abundance, Carbon Monoxide, Chemical Composition, Radio Emission, Spatial Distribution
Scientific paper
A two-component dust model is suggested to explain the infrared emission from planetary nebulae. A cold dust component located in the extensive remnant of the red-giant envelope exterior to the visible nebula is responsible for the far-infrared emission. A warm dust component, which is condensed after the formation of the planetary nebula and confined within the ionized gas shell, emits most of the near- and mid-infrared radiation. The observations of NGC 7027 are shown to be consistent with such a model. The correlation of silicate emission in several planetary nebulae with an approximately + 1 spectral index at low radio frequencies suggests that both the silicate and radio emissions originate from the remnant of the circumstellar envelope of the precursor star and are observable only while the planetary nebula is young. It is argued that oxygen-rich stars as well as carbon-rich stars can be progenitors of planetary nebulae.
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