Abstract
After the star has lost most of its envelope while on the asymptotic giant branch (AGB), and before it is seen as a planetary nebula, the object is in a transition phase, called post-AGB or pre-planetary nebula (PPN). The characteristics of PPNe show that the properties of PNe are already in place at the end of the AGB phase. Moreover, the post-AGBs surrounded by discs are found to be all intermediate period binary systems, while PPNe show torus, outflows and jets which are most likely signature of binarity.
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- 1.
Historically, the name “proto-planetary nebula” was more commonly used (e.g., Kwok 1993) however, as highlighted by Sahai et al. (2005), the term “proto-planetary” is now widely used to refer to discs around pre-main sequence stars. As such, the continued use of proto-planetary nebula unfortunately has ambiguous implications (especially when one also folds in the inherently confusing nature of the misnomer “planetary nebula” to begin with!), and it is therefore important to use the (slightly) more favourable name “pre-planetary nebula”.
- 2.
One should note, however, that the Red Rectangle is atypical is having a nebula surrounding it!
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Boffin, H.M.J., Jones, D. (2019). Post-AGBs and Pre-planetary Nebulae. In: The Importance of Binaries in the Formation and Evolution of Planetary Nebulae. SpringerBriefs in Astronomy. Springer, Cham. https://doi.org/10.1007/978-3-030-25059-1_7
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DOI: https://doi.org/10.1007/978-3-030-25059-1_7
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