Spectral Classification of Planetary Nebula Wolf-Rayet Central Stars

Details Spectral Classification of Planetary Nebula Wolf-Rayet Central Stars Spectral Classification of Planetary Nebula Wolf-Rayet Central Stars

Feb 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999noao.prop..162j&link_type=abstract

NOAO Proposal ID #1999A-0162

Computer Science

Scientific paper

We will obtain medium resolution spectra of ~36 planetary nebula central stars with emission-lines indicative of winds and mass loss (e.g. WR stars). The immediate purpose is to determine a temperature sequence, through classification and atmosphere modeling, for those hydrogen deficient central stars of PN having winds. Temperatures will be compared to a similar sample in the SMC where the metallicity is lower by a factor of ~5 to test the predictions of stellar wind theory:
that lower metallicity stars develop weaker radiationally driven winds, and
that PN central stars behave like their Population I WR counterparts where the metallicity effect (item 1 above) is seen. For 3 PN in the LMC, no metallicity effect is evident.
This proposal is part of a larger investigation in which the evolutionary status and sequencing of emission-line stars in PN is being evaluated. PN central stars offer two advantages over their massive Pop I (WR) counterparts: their progenitor abundances can be derived from a nebular analysis, and their status in time can be estimated from the nebular expansion age. Thus, it should be possible, by studying PN in galaxies of differing metallicity, to ascertain the effects of metallicity on the development and strength of winds in hot stars, and the temperature and gravity conditions that allow a wind to form.

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