Volume 444, Number 3, December IV 2005
|Page(s)||861 - 870|
|Section||Interstellar and circumstellar matter|
|Published online||05 December 2005|
Abundances in planetary nebulae: Mz 3
Kapteyn Astronomical Institute, PO Box 800, 9700 AV Groningen, The Netherlands e-mail: email@example.com
2 Indian Institute of Astrophysics, Koramangala II Block, Bangalore 560034, India
Accepted: 22 August 2005
ISO spectra of the bipolar planetary nebula Mz 3 are used to determine the element abundances in the bright lobes of the nebula. The ISO spectra alone are sufficient to determine nitrogen, neon, argon, sulfur and iron abundances. These spectra are combined with spectra in the visual wavelength region (taken from the literature) to obtain an extinction corrected spectrum which is used to determine the abundance of oxygen and some other elements using a classical determination. We have tried abundance determination using photoionization modeling using cloudy, which is essential for determining the helium, silicon and chlorine abundances. It was found difficult to model the entire spectrum. New information about the central star could be determined. The abundances determined are found to differ somewhat from earlier results using only visual spectra. The reasons for this difference are discussed. An elevated helium abundance is found, agreeing with the determination of Smith 2003. Taken together with the high nitrogen abundance found, it is concluded that the exciting star of Mz 3 had a high progenitor mass.
Key words: ISM: abundances / stars: AGB and post-AGB / planetary nebulae: individual: Mz 3
© ESO, 2005
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