Are planetary nebulae derived from multiple evolutionary scenarios?

Frew, David J.; Parker, Quentin A.

doi:10.1017/s1743921312010940

Cited by 4 publications

(4 citation statements)

References 38 publications

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“…They further suggest that in a several months long outburst a main-sequence companion accretes mass from an AGB star and launches jets, that both shape the bipolar PN and powered an ILOT event. The ILOT scenario was mentioned in relation to more PNe (Frew & Parker 2012;Boumis & Meaburn 2013;Clyne et al 2014;Frew et al 2016). Corradi et al (2014a) raise the possibility that the YSO bipolar nebula Ou4 was formed in an ILOT event, as Boumis & Meaburn (2013) suggest for the PN KjPn 8 that has a similar morphology.…”

Section: Intermediate-luminosity Optical Transients (Ilots)mentioning

confidence: 99%

The jet feedback mechanism (JFM) in stars, galaxies and clusters

Soker

2016

New Astronomy Reviews

149

106

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I review the influence jets and the bubbles they inflate might have on their ambient gas as they operate through a negative jet feedback mechanism (JFM). I discuss astrophysical systems where jets are observed to influence the ambient gas, in many cases by inflating large, hot, and low-density bubbles, and systems where the operation of the JFM is still a theoretical suggestion. The first group includes cooling flows in galaxies and clusters of galaxies, star-forming galaxies, young stellar objects, and bipolar planetary nebulae. The second group includes core collapse supernovae, the common envelope evolution, the grazing envelope evolution, and intermediate luminosity optical transients. The suggestion that the JFM operates in these four types of systems is based on the assumption that jets are much more common than what is inferred from objects where they are directly observed. Common to all eight types of systems reviewed here is the presence of a compact object inside an extended ambient gas. The ambient gas serves as a potential reservoir of mass to be accreted on to the compact object. If the compact object launches jets as it accretes mass, the jets might reduce the accretion rate as they deposit energy to the ambient gas, or even remove the entire ambient gas, hence closing a negative feedback cycle.

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Section: Intermediate-luminosity Optical Transients (Ilots)mentioning

confidence: 99%

The jet feedback mechanism (JFM) in stars, galaxies and clusters

Soker

2016

New Astronomy Reviews

149

106

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“…From the IRAS two-colour diagram, they find that WELS are shifted to bluer colours than the other [WR] PNe. Frew & Parker (2012) show that WELS have larger scale height compared to other many CS classes and consequently they rise from low mass progenitor stars.…”

Section: Introductionmentioning

confidence: 89%

“…These lines are indistinguishable in width from the nebular lines, although on low dispersion spectra the group of lines around 4650Å and the C IV doublet around 5805Å may appear to be broad features. Frew & Parker (2012) noted that the characteristics WELS recombination lines such as C IIII, C IIV and N IIII were also observed in some massive O-type stars, as well as in low-mass X-ray binaries and cataclysmic variables. Corradi et al (2011) observed these C IIII, C IIV and N IIII emission lines in the spectrum of the close binary CS of the high-excited PN IPHASX J194359.5+170901.…”

Section: Introductionmentioning

confidence: 97%

Problems for the WELS classification of planetary nebula central stars: self-consistent nebular modelling of four candidates

Basurah

Ali

Dopita

et al. 2016

Mon. Not. R. Astron. Soc.

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We present integral field unit (IFU) spectroscopy and self-consistent photoionisation modelling for a sample of four southern Galactic planetary nebulae (PNe) with supposed weak emission-line (WEL) central stars. The Wide Field Spectrograph (WiFeS) on the ANU 2.3 m telescope has been used to provide IFU spectroscopy for NGC 3211, NGC 5979, My 60, and M 4-2 covering the spectral range of 3400-7000Å. All objects are high excitation non-Type I PNe, with strong He II emission, strong [Ne V] emission, and weak low-excitation lines. They all appear to be predominantly optically-thin nebulae excited by central stars with T eff > 10 5 K. Three PNe of the sample have central stars which have been previously classified as weak emission-line stars (WELS), and the fourth also shows the characteristic recombination lines of a WELS. However, the spatially-resolved spectroscopy shows that rather than arising in the central star, the C IV and N III recombination line emission is distributed in the nebula, and in some cases concentrated in discrete nebular knots. This may suggest that the WELS classification is spurious, and that, rather, these lines arise from (possibly chemically enriched) pockets of nebular gas. Indeed, from careful background subtraction we were able to identify three of the sample as being hydrogen rich O(H)-Type. We have constructed fully self-consistent photoionization models for each object. This allows us to independently determine the chemical abundances in the nebulae, to provide new model-dependent distance estimates, and to place the central stars on the H-R diagram. All four PNe have similar initial mass (1.5 < M/M ⊙ < 2.0) and are at a similar evolutionary stage.

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“…This, and their use as key Galactic probes, provides strong motivation to hunt for them. Much progress has been made since the major Galactic PNe discoveries report by Parker et al (2006) and Miszalski et al (2008), as well as obtaining a better understanding of the different evolutionary pathways that can lead to PNe formation, e.g., Stanghellini and Pasquali, (1995) and Frew and Parker (2012).…”

Section: Basic Pne Propertiesmentioning

confidence: 99%

Planetary nebulae and how to find them: A concise review

Parker

2022

Front. Astron. Space Sci.

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This review provides useful background and information on how we find, vet and compile Planetary Nebulae (PNe) candidates and verify them. It presents a summary of the known Galactic PNe population and their curation in the Hong Kong/AAO/Strasbourg/Hα PNe catalogue, “HASH”. It is a simple introduction for anyone interested in working with PNe, including postgraduate students entering the field and for more general interest too.

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Are planetary nebulae derived from multiple evolutionary scenarios?

Cited by 4 publications

References 38 publications

The jet feedback mechanism (JFM) in stars, galaxies and clusters

The jet feedback mechanism (JFM) in stars, galaxies and clusters

Problems for the WELS classification of planetary nebula central stars: self-consistent nebular modelling of four candidates

Planetary nebulae and how to find them: A concise review

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