On the evolutionary link between white dwarfs and central stars of planetary nebulae - NLTE analysis of PG 1144 + 005

Details On the evolutionary link between white dwarfs and central stars of planetary nebulae - NLTE analysis of PG 1144 + 005 On the evolutionary link between white dwarfs and central stars of planetary nebulae - NLTE analysis of PG 1144 + 005

Jul 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...247..476w&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 247, no. 2, July 1991, p. 476-486.

Astronomy and Astrophysics

Astrophysics

42

Atmospheric Models, Planetary Nebulae, Stellar Atmospheres, Stellar Evolution, Stellar Spectra, White Dwarf Stars, Abundance, Emission Spectra, Line Spectra, Nitrogen, Radiative Transfer

Scientific paper

Line-blanketed non-LTE (NLTE) model atmospheres are used to study the optical spectra of the hydrogen-deficient prewhite dwarf PG 1144 + 005 by means of a spectral analysis. The star is compared to a prototype PG 1159 star for the analysis, and the stellar parameters of the PG 1144 dwarf show that the N/O ratio is indicative of very strong nitrogen emission. The high N/O ratio suggests that N is not present in the helium-buffer layer, meaning that PG 1144 does not fit the scenario proposed by Iben et al. (1983). Based on a spectroscopic comparison of central stars of planetary nebulae (CSPN), the existence of N-rich stars is explained in relation to two evolutionary sequences. The sequences consider either N-rich or N-poor links, and it is suggested that the sequences can be linked because N-rich layers can be removed by continuing mass loss during the evolutionary process. Abundance determinations of N-rich objects are required for future clarification of evolutionary stages in these stars.

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