The effect of dust in planetary nebulae on determinations of Zanstra temperatures of the central stars

Details The effect of dust in planetary nebulae on determinations of Zanstra temperatures of the central stars The effect of dust in planetary nebulae on determinations of Zanstra temperatures of the central stars

Jan 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a....94..109h&link_type=abstract

Astronomy and Astrophysics, vol. 94, no. 1, Jan. 1981, p. 109-115.

Astronomy and Astrophysics

Astrophysics

24

Cosmic Dust, Emission Spectra, Line Spectra, Planetary Nebulae, Stellar Temperature, Far Ultraviolet Radiation, H Lines, Helium, Opacity, Stellar Evolution, Ultraviolet Absorption

Scientific paper

The peak effective temperatures of planetary nuclei predicted from stellar evolution calculations are considerably greater than temperatures determined from observations. It is shown that absorption of ionizing radiation by dust in a planetary nebula can result in Zanstra temperatures that may considerably underestimate the actual temperature of the central star. For example, in a planetary nucleus model with effective temperature of 200,000 K, log g = 7, it is found that the Zanstra temperature determined from the H-beta emission flux can be reduced to a value as low as 91,000 K for a dust-to-gas mass ratio of not greater than 0.01, if the dust is strongly absorbing in the far UV. The presence of dust also produces discordances among the Zanstra temperatures determined from H I, He I, and He II emission lines. However, even when dust is present, the nebular emission line ratio 4686/H-beta provides a means for estimating temperatures of exciting stars reliably.

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