HM Sagittae as a young planetary nebula

Details HM Sagittae as a young planetary nebula HM Sagittae as a young planetary nebula

Apr 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...229..187k&link_type=abstract

Astrophysical Journal, Part 1, vol. 229, Apr. 1, 1979, p. 187-195. Research supported by the National Research Council of Canad

Astronomy and Astrophysics

Astrophysics

45

Emission Spectra, Planetary Nebulae, Red Giant Stars, Stellar Models, Stellar Spectra, Stellar Winds, Distance, Forbidden Bands, Infrared Spectra, Optical Emission Spectroscopy, Radio Spectra, Stellar Envelopes, Stellar Mass Ejection

Scientific paper

HM Sagittae is suggested to be a very young planetary nebula recently transformed from a red-giant star through continuous mass loss. The observational data for HM Sagittae are analyzed in terms of the interacting stellar wind model of planetary nebula formation. The density in the newly formed shell is found to be at least 5 x 10 to the 7th/cu cm, a value considerably higher than that found by the conventional analysis, which assumes a single-component homogeneous nebula. The low observed mass is shown to be consistent with the interacting stellar wind model but not consistent with the conventional sudden-ejection model of planetary nebula formation.

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