Alternative methods for determination of the temperature of central stars of planetary nebulae

Details Alternative methods for determination of the temperature of central stars of planetary nebulae Alternative methods for determination of the temperature of central stars of planetary nebulae

Mar 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992ipesprept.....e&link_type=abstract

M.S. Thesis Instituto de Pesquisas Espaciais, Sao Jose dos Campos (Brazil).

Statistics

Applications

Planetary Nebulae, Stellar Temperature, Helium, Hydrogen, Stellar Spectra

Scientific paper

This work presents the formulation and application of three methods for determining the temperature of central stars in planetary nebulae. The methods are based on global spectroscopic indices for comparing objects with models. The spectroscopic data are taken from the literature, while models were calculated with the CLOUDY code. The three methods are: the Ir method compares the ratio of helium to hydrogen lines; the S-N1/2 method generalizes the energy balance method for different metalicity classes and different gas densities; the TIN method makes a direct comparison between the spectroscopic indices of the model and the object, minimizing their differences. In this method the chemical abundances of the main elements are calculated. The Ir method was applied to 78 objects; the S-N1/2 method was applied to 85 objects while the TIN method was used upon 8 nebulae. The results are discussed and compared to other determinations in the literature. One of the main conclusions is that only about half of the objects are optically thick. Finally, future developments and applications are suggested.

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