Ground-based and IRAS observations of compact planetary nebulae

Details Ground-based and IRAS observations of compact planetary nebulae Ground-based and IRAS observations of compact planetary nebulae

Apr 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...303..451k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 303, April 1, 1986, p. 451-464. NSERC-supported research.

Astronomy and Astrophysics

Astronomy

47

Astronomical Spectroscopy, Density Distribution, Infrared Spectroscopy, Planetary Nebulae, Stellar Evolution, Asymptotic Giant Branch Stars, Cosmic Dust, Far Infrared Radiation, Giant Stars, Infrared Astronomy Satellite, Optical Thickness, Radiant Flux Density, Spaceborne Astronomy, Stellar Envelopes

Scientific paper

A group of compact planetary nebulae suspected of being young objects from their radio properties were observed in the infrared using the Canada-France-Hawaii Telescope. Combining these results with the data from the IRAS satellite, it is found that most have far-infrared excesses with color temperatures of about 200 K. The free-free emission components are clearly distinguished from the dust components and are consistent with the levels of continuum emission expected from radio measurements. For the first time, the total bolometric fluxes of the nebulae have been measured, and the results suggest that the dust in these compact nebulae are heated by direct starlight rather than by nebular Lyman-alpha photons. Also found is a clear correlation between the dust optical depth and the radio surface brightness temperature, suggesting that the dust optical depth is monotonically decreasing with age and the dust component is dispersing into the interstellar medium. The similarity of the infrared spectra of these young nebulae with those of late asymptotic giant branch stars supports the suggestion of Kwok (1980) that the far-infrared dust emission of planetary nebulae originates from the remnants of the circumstellar envelopes of their red giant progenitors.

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