Morphology vs. physical properties: some comments and questions

By R. Corradi. 2000

349 citations recorded by the source corpus.

Some of the correlations between morphological and other physical properties of planetary nebulae (PNe) are reviewed. In particular, the finding that bipolar (b) PNe have more massive progenitors than the other morphological classes is discussed in detail. Earlier results are confirmed; including all the various sources of uncertainty, the Galactic distribution of objects indicate that b PNe are formed by stars with initial masses >1.3 solar masses, while elliptical (e) PNe by progenitors with masses <1.3 solar masses. Recent results for the chemical abundances of b and e PNe and their orientation within the Galaxy are also presented. Finally, the key role in the discussion of the formation of b PNe played by detached binary systems such as symbiotic stars is briefly discussed.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/b44df8c9237329c4b73e42868c93f776f7155bf6

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Citations in the corpus

Is HE 0107–5240 A Primordial Star? The Characteristics of Extremely Metal-Poor Carbon-Rich Stars (2004, background): “The models enter the TPAGB evolutionary phase in the same fashion as do model stars of younger populations (FII00); successive third dredge-up episodes increase the surface C abundance and lead to a large C/N abundance ratio.”
Common envelope evolution: where we stand and how we can move forward (2012, background): “Approximately one in five planetary nebulae (PNe) are ejected common envelopes (Han et al. 1995; Bond 2000; Miszalski et al. 2009b).”
Dawes Review 6: The Impact of Companions on Stellar Evolution (2016, background): “…of PN formation must be able to explain: (1) At least 15–20% of PNe have post-CE central stars (Section 4.2.2) in their centres, detected by light variability due to irradiation, ellipsoidal effects or eclipses in the close binaries (see Figure 9 and Section 3; Bond, 2000; Miszalski et al., 2009a).”