Models for the planetary nebulae NGC 4361 and NGC 1535 Influence of the stellar wind on the nebular ionization

Details Models for the planetary nebulae NGC 4361 and NGC 1535 Influence of the stellar wind on the nebular ionization Models for the planetary nebulae NGC 4361 and NGC 1535 Influence of the stellar wind on the nebular ionization

Jan 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985a%26a...142..461a&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 142, no. 2, Jan. 1985, p. 461-475. Sponsorship: Deutsche Forschungsgemeinschaf

Astronomy and Astrophysics

Astrophysics

35

Iue, Photoionization, Planetary Nebulae, Stellar Evolution, Stellar Models, Stellar Winds, Electron Density (Concentration), Electron Energy, Hertzsprung-Russell Diagram, Red Giant Stars, Ultraviolet Spectra, White Dwarf Stars

Scientific paper

Model atmospheres fitted to line profiles of the central stars (Méndez et al., 1981) are used to construct nebular ionization models for the planetary nebulae NGC 4361 and 1535. For NGC 4361 the optical and IUE nebular emission lines are reproduced satisfactorily well. For NGC 1535 the model atmospheres only emit less than 10-3 of the number of He+ ionizing photons which are necessary to explain the observed nebular He II emission. The IUE spectrum of NGC 1535 shows P Cyg profiles of N V and O V and, in contrast, NGC 4361 does not. The authors find that a stellar wind with electron temperature Te = 3×105K and mass-loss-rate M= 10-7M_sun;/a explains the P Cyg profiles and provides the required number of He+ ionizing photons by thermal emission. Consequently, the He II Zanstra temperature of NGC 1535 does not represent the effective temperature of the central star.

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