Origin of planetary nebulae - Morphology, carbon-to-oxygen abundance ratios, and central star multiplicity

Zuckerman, B.; Aller, L. H.

doi:10.1086/163943

Cited by 145 publications

(85 citation statements)

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“…There is still no conclusive theory capable of explaining why more than 80% of known planetary nebulae (PNe) have bipolar and non-spherically symmetric structures (Zuckerman & Aller 1986;Stanghellini et al 1993;Corradi & Schwarz 1995). An overview of the mechanisms that may shape PNe is given by Balick & Frank (2002).…”

Section: Introductionmentioning

confidence: 99%

Magnetic fields in central stars of planetary nebulae?

Jordan

Bagnulo

Werner

et al. 2012

A&A

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Context. Most planetary nebulae have bipolar or other non-spherically symmetric shapes. Magnetic fields in the central star may be responsible for this lack of symmetry, but observational studies published to date have reported contradictory results. Aims. We search for correlations between a magnetic field and departures from the spherical geometry of the envelopes of planetary nebulae. Methods. We determine the magnetic fields from spectropolarimetric observations of ten central stars of planetary nebulae. The results of the analysis of the observations of four stars were previously presented and discussed in the literature, while the observations of six stars, plus additional measurements of a star previously observed, are presented here for the first time.Results. All our determinations of magnetic field in the central planetary nebulae are consistent with null results. Our field measurements have a typical error bar of 150-300 G. Previous spurious field detections using data acquired with FORS1 (FOcal Reducer and low dispersion Spectrograph) of the Unit Telescope 1 (UT1) of the Very Large Telescope (VLT) were probably due to the use of different wavelength calibration solutions for frames obtained at different position angles of the retarder waveplate. Conclusions. There is currently no observational evidence of magnetic fields with a strength of the order of hundreds Gauss or higher in the central stars of planetary nebulae.

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Section: Introductionmentioning

confidence: 99%

Magnetic fields in central stars of planetary nebulae?

Jordan

Bagnulo

Werner

et al. 2012

A&A

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“…The origin of the axisymmetric morphology of young PNe has long been an unresolved issue. In classification of PNe based on their morphology, Zuckerman & Aller (1986) and Soker (1997) found that a large majority of PNe have nonspherical shapes, some indicating extreme bipolar or axisymmetric structure. Such structures could be generated by strong bipolar outflows during the late asymptotic giant branch (AGB) or post-AGB phase and may be transient phenomena (Kwok et al 2000).…”

Section: Introductionmentioning

confidence: 99%

Evidence for a Binary Origin of the Young Planetary Nebula Hubble 12

Hsia

2006

Astron J

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Young planetary nebulae play an important role in stellar evolution when intermediate-to low-mass stars (0.8-8 M ) evolve from the proto-planetary nebula phase to the planetary nebula phase. Many young planetary nebulae display distinct bipolar structures as they evolve away from the proto-planetary nebula phase. One possible cause of their bipolarity could be a binary origin for their energy source. Here we report on our detailed investigation of the young planetary nebula Hubble 12, which is well known for its extended hourglass-like envelope. We present evidence with time-series photometric observations for the existence of an eclipsing binary at the center of Hubble 12. In addition, low-resolution spectra of the central source show absorption features such as CN, G band, and Mg b, which can be suggestive of a low-mass nature for the secondary component.

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“…In some cases, the binary model with its various aspects (Livio et al 1979;Morris 1981; and more recently Pilyugin 1986, 1989;Morris 1987Morris , 1990Soker and Livio 1989) does appear capable to explain both the ejection of gas and the bipolarity. Nevertheless, some problems remain with such a hypothesis (Zuckerman and Aller 1986;Pascoli 1987a). In any way, it seems very unlikely that the binary model applies to all the encountered cases of bipolar PPNe and PNe.…”

Section: Introductionmentioning

confidence: 99%

On the shaping of circumstellar envelopes

Pascoli¹,

Leclercq²,

Poulain³

1992

PASP

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ABSTRACT. In this paper, we examine the evolutionary process of expansion of a magnetized ring of cool matter ejected from a red giant. The subsequent formation of a circumstellar shell or preplanetary nebula is also analyzed. The velocity, density, and magnetic field are calculated along a time sequence, on a large two-dimensional grid of points close to and far away from the star. Owing to long-range forces such as thermal pressure gradients and magnetic stresses, the velocity field becomes a linear function of the distance. The latitudinal dependence of this function is poor, while conversely the density distribution is clearly aspheric. The magnetic field intensity at a distance -10 15 -10 16 cm is in good agreement with the observational data. The isophotes are plotted and compared to observational contours obtained from the literature. The filamentary structure appearance and its stability within the envelope are also discussed.

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Origin of planetary nebulae - Morphology, carbon-to-oxygen abundance ratios, and central star multiplicity

Cited by 145 publications

References 0 publications

Magnetic fields in central stars of planetary nebulae?

Magnetic fields in central stars of planetary nebulae?

Evidence for a Binary Origin of the Young Planetary Nebula Hubble 12

On the shaping of circumstellar envelopes

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