Dust in planetary nebulae

Journal Article · Sat Mar 01 04:00:00 EST 1980 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/157777· OSTI ID:5407523

Kwok, S

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 ward 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 consisten 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 th 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.

• Research Organization: Herzberg Institute of Astrophysics, National Research Council of Canada
• OSTI ID: 5407523
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 236:2; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
CHEMICAL COMPOSITION
COSMIC DUST
DUSTS
ELECTROMAGNETIC RADIATION
EMISSION
GIANT STARS
INFRARED RADIATION
INTERSTELLAR GRAINS
NEBULAE
OXYGEN COMPOUNDS
PARTICLES
PLANETARY NEBULAE
RADIATION FLUX
RADIATIONS
RED GIANT STARS
SILICATES
SILICON COMPOUNDS
STAR EVOLUTION
STARS