Morphology and Evolution of Galactic and Magellanic Cloud Planetary Nebulae
arXiv:astro-ph/9906188 · doi:10.1023/A:1002632110017
Abstract
Planetary nebulae (PNe) exist in a range of different morphologies, from very simple and symmetric round shells, to elliptical, bipolar, and even quadrupolar shapes. They present extremely complex ensembles of filaments, knots, ansae, and shell multiplicity. It is then overwhelmingly complicated to derive reasonable evolutionary paths to justify the observed shapes of PNe. The confrontation between the evolution of the shells and that of the central stars is needed to understand the origin of the morphological variety. We present some background and recent results on the correlations between PN morphology and PN nuclei (PNNi) evolution, including a study on the Magellanic Cloud PNe.
arXiv comment8 pages, 5 figures; proceedings of ``Astrophysical Dynamics. Conference to commemorate the work of Franz D. Kahn''; Evora, April 14-16 1999; to be published in Ap&SS (Kluwer)
References in corpus (1)
Cited by in corpus (3)
- Spitzer IRAC observations of newly-discovered planetary nebulae from the Macquarie-AAO-Strasbourg H-alpha Planetary Nebula Project
- Multi-wavelength diagnostic properties of Galactic Planetary Nebulae detected by GLIMPSE-I
- The Low- and Intermediate-Mass Stellar Population in the Small Magellanic Cloud: The Central Stars of Planetary Nebulae