Hydrostatic evolutionary sequences for the nuclei of planetary nebulae

Details Hydrostatic evolutionary sequences for the nuclei of planetary nebulae Hydrostatic evolutionary sequences for the nuclei of planetary nebulae

Aug 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...307..659w&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 307, Aug. 15, 1986, p. 659-674.

Astronomy and Astrophysics

Astrophysics

273

Hydrostatics, Planetary Nebulae, Stellar Evolution, Asymptotic Giant Branch Stars, Helium, Hydrogen, Nuclei, Stellar Mass Ejection, Stellar Models

Scientific paper

This paper describes a set of evolutionary calculations for nuclei of planetary nebulae. The properties of the nuclei are studied as a function of the following three input parameters: (1) mass of the nucleus, which is set equal to 0.60, 0.70, 0.76, and 0.89 M_sun;; (2) departure phase from the asymptotic giant branch (AGB), which is set at four equally spaced values within the helium shell flash cycle; and (3) mass loss, which takes a range of forms. The authors argue that every AGB star capable of producing a core mass greater than 0.86 M_sun; will produce a planetary nebula with a helium-rich nucleus. Such nuclei will evolve through the planetary nebula phase burning helium before cooling off to become non-DA white dwarfs.

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