Density contrast shell models for the planetary nebula IC 2165

Hyung, Siek

doi:10.1086/191860

Cited by 62 publications

(64 citation statements)

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“…The data used were taken from the electronic emissionline catalogue for planetary nebulae by Kaler et al (1997), from Kingsburgh & English (1992) and from the spectral survey of high surface brightness planetaries by Hyung, Aller, Feibelman and collaborators (Aller & Hyung 1995;Aller et al 1996;Feibelman et al 1994Feibelman et al , 1996Hyung 1994;Hyung & Aller 1995a,b, 1996, 1997a,b, 1998Hyung et al 1993Hyung et al , 1994aHyung et al ,b,c, 1995Hyung et al , 1997Hyung et al , 1999aHyung et al ,b, 2000Hyung et al , 2001Keyes et al 1990). Instead of comparing directly the derived densities, as has been done by other authors, what implies in discarding all line ratios close or beyond the saturation limits at low and high densities, we have compared the line ratios themselves with one another.…”

Section: Discussionmentioning

confidence: 99%

Study of electron density in planetary nebulae

Copetti

Writzl

2002

A&A

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Abstract. We present a comparison of electron density estimates for planetary nebulae based on different emissionline ratios. We have considered the density indicators. The observational data were extracted from the literature. We have found systematic deviations from the density homogeneous models, in the sense that:We argue that the lower [O ii] density estimates are likely due to errors in the atomic parameters used.

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Section: Discussionmentioning

confidence: 99%

Study of electron density in planetary nebulae

Copetti

Writzl

2002

A&A

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“…Using the double-beam spectrograph mounted on the ANU 2.3 m telescope, Kingsburgh & English (1992) ple of Galactic PNe and found that electron densities derived from the two ratios were in excellent agreement. On the other hand, a very different result was obtained by Meatheringham & Dopita (1991) Aller et al 1996;Feibelman et al 1994Feibelman et al , 1996Hyung 1994;Hyung & Aller 1995a,b, 1996, 1997a,b, 1998Hyung et al 1993Hyung et al , 1994aHyung et al ,b,c, 1995Hyung et al , 1997Hyung et al , 1999aHyung et al ,b, 2000Hyung et al , 2001Keyes et al 1990;Keenan et al 1993Keenan et al , 1996Keenan et al , 1997 they determined simultaneously electron densities and temperatures using a number of plasma diagnostic lines in the optical and ultraviolet and found that overall the data yielded compatible and consistent results. More recently, Copetti & Writzl (2002), using data published in the literature, compared the observed line ratios for a number of density-diagnostics, instead of densities deduced from them, thus avoiding discarding measurements that yield ratios close to or beyond the the low-or high-N e limits.…”

Section: Introductionmentioning

confidence: 90%

A reexamination of electron density diagnostics for ionized gaseous nebulae

Wang¹,

Liu²,

Zhang³

et al. 2004

A&A

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Abstract. We present a comparison of electron densities derived from optical forbidden line diagnostic ratios for a sample of over a hundred nebulae. We consider four density indicators, theand [Ar ] λ4711/λ4740 doublet ratios. Except for a few H  regions for which data from the literature were used, diagnostic line ratios were derived from our own high quality spectra. For the [O ] λ3729/λ3726 doublet ratio, we find that our default atomic data set, consisting of transition probabilities from Zeippen (1982)

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“…Hence, we derive all these ionic abundances using the densities and temperatures from Benjamin et al (1999). In DdDm 1 and IC 2165 we replace our computed He + abundances (He + /H + = 0.041 and 0.042) with the average of the He + abundances derived from the He i λλ4471, 5876 lines by Hyung (1994) and Wesson et al (2005), respectively. These authors suggest that the low values implied by the λ6678 line could be due to underlying absorption.…”

Section: Ionic Abundancesmentioning

confidence: 99%

C/O Abundance Ratios, Iron Depletions, and Infrared Dust Features in Galactic Planetary Nebulae

Delgado-Inglada

Rodríguez

2014

ApJ

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We study the dust present in 56 Galactic planetary nebulae (PNe) through their iron depletion factors, their C/O abundance ratios (in 51 objects), and the dust features that appear in their infrared spectra (for 33 objects). Our sample objects have deep optical spectra of good quality, and most of them also have ultraviolet observations. We use these observations to derive the iron abundances and the C/O abundance ratios in a homogeneous way for all the objects. We compile detections of infrared dust features from the literature and we analyze the available Spitzer/IRS spectra. Most of the PNe have C/O ratios below one and show crystalline silicates in their infrared spectra. The PNe with silicates have C/O < 1, with the exception of Cn 1-5. Most of the PNe with dust features related to C-rich environments (SiC or the 30 μm feature usually associated to MgS) have C/O 0.8. Polycyclic aromatic hydrocarbons are detected over the full range of C/O values, including 6 objects that also show silicates. Iron abundances are low in all the objects, implying that more than 90% of their iron atoms are deposited into dust grains. The range of iron depletions in the sample covers about two orders of magnitude, and we find that the highest depletion factors are found in C-rich objects with SiC or the 30 μm feature in their infrared spectra, whereas some of the O-rich objects with silicates show the lowest depletion factors.

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Density contrast shell models for the planetary nebula IC 2165

Cited by 62 publications

References 0 publications

Study of electron density in planetary nebulae

Study of electron density in planetary nebulae

A reexamination of electron density diagnostics for ionized gaseous nebulae

C/O Abundance Ratios, Iron Depletions, and Infrared Dust Features in Galactic Planetary Nebulae

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