Abundances of Planetary Nebula NGC 5315

Pottasch, [No Value]; Beintema, D. A.; Salas, JB; Koornneef, J.; Feibelman, W. A.

doi:10.1051/0004-6361:20020986

Cited by 49 publications

(74 citation statements)

References 19 publications

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“…2). This has previously been detected for NGC 7027 (Bernard Salas et al 2001), NGC 6302 (Pottasch & Beintema 1999) and NGC 6537 (Pottasch et al 2000). A simple picture of a planetary nebula is that close to the central star there exist more high energy UV photons than in the outer regions.…”

Section: Discussionmentioning

confidence: 56%

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An ISO and IUE study of planetary nebula NGC 2440

Salas

Pottasch²,

Feibelman

et al. 2002

A&A

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Abstract. The infrared and ultraviolet spectra of planetary nebula NGC 2440 are presented. The observations were made by the Infrared Space Observatory (ISO) and the International Ultraviolet Explorer (IUE). These data, in conjunction with published optical observations have been used to derive electron temperature and density. The electron temperature increases with increasing ionization potential, from 11 000 to 18 000 K. The electron density has a constant value of 4500 cm −3 in agreement with previous determinations. The chemical abundance has been derived for the following elements; helium, carbon, nitrogen, oxygen, neon, sulfur and argon. The ionization correction factor turns out to be very small for all species except sulfur.

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Section: Discussionmentioning

confidence: 56%

“…This comparison is shown in Table 1. The SWS and IRAS fluxes (Pottasch et al 2000) are shown in Cols. 4 and 5. In the last column the scale factor to reproduce the IRAS measurements (basically F iras /F sws ) is given.…”

Section: Aperture Correctionsmentioning

confidence: 99%

An ISO and IUE study of planetary nebula NGC 2440

Salas

Pottasch²,

Feibelman

et al. 2002

A&A

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“…The reasons for this have been discussed in earlier studies (e.g. see Pottasch & Beintema 1999; Pottasch et al 2000Pottasch et al , 2001Bernard Salas et al 2001), and can be summarized as follows.…”

Section: Introductionmentioning

confidence: 85%

Abundances in the planetary nebula NGC 6210

Pottasch¹,

Bernard─Salas

Roellig

2009

A&A

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The spectra of the planetary nebula NGC 6210 is reanalysed using spectral measurements made in the mid-infrared with the Spitzer Space Telescope and the Infrared Space Observatory. The aim is to determine the chemical composition of this object. We also make use of IUE and ground based spectra. Abundances determined from the mid-infrared lines, which are insensitive to electron temperature, are used as the basis for the determination of the composition, which is found to differ somewhat from earlier results. The abundances found, especially the low value of helium and oxygen, indicate that the central star was originally of rather low mass, probably ≤1 M . Abundances of phosphorus, iron, silicon, sodium, potassium and chlorine have been determined, some for the first time in this nebula. The electron temperature in this nebula is constant. The temperature, radius and luminosity of the central star is also discussed. It is shown that the luminosity is consistent with that predicted for a star of 0.9 M . But the predicted nebular age is inconsistent with the observed kinetic age.

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“…Pottasch 2003, private communication). When the results calculated from ISO data are compared to other recent abundance determinations, large errors (sometimes of factors two to three) are found (see Pottasch et al 2000 for an example).…”

Section: The Observationsmentioning

confidence: 99%

“…Pottasch 2003, private communication). These abundances will be much more accurate than just using visual data alone because infrared data do not depend on electron temperature, the number of ions observed may double, which reduces the uncertainty in the ionisation correction factor substantially and extinction corrections may be determined in an independent way (Pottasch, Beintema, & Feibelman 2000). Indeed, for the cases of neon, oxygen and argon, ionisation correction factors are no longer needed (S.R.…”

Section: The Observationsmentioning

confidence: 99%

AGB Stars and the Observed Abundance of Neon in Planetary Nebulae

Karakas

Lattanzio

2003

Publ. – Astron. Soc. Aust

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Asymptotic giant branch stars are expected to produce 22 Ne through the combined H and He burning that operates during their thermally pulsing evolution. However, observationally there is a fairly tight correlation between the O and Ne abundances as measured in planetary nebulae in various populations. In this paper we use recent detailed stellar evolutionary calculations for compositions appropriate to the Galaxy and the Large Magellanic Cloud, in an attempt to determine if the models are consistent with the observed abundances. We show that there is only a narrow range in stellar mass, about 2 to 4 M ⊙ (lower for lower [Fe/H]) where 22 Ne is produced in sufficient quantities to affect the total observed elemental neon abundance, which is mostly 20 Ne. The models appear to be consistent with the observations, but a more thorough analysis is required.

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Abundances of Planetary Nebula NGC 5315

Cited by 49 publications

References 19 publications

An ISO and IUE study of planetary nebula NGC 2440

An ISO and IUE study of planetary nebula NGC 2440

Abundances in the planetary nebula NGC 6210

AGB Stars and the Observed Abundance of Neon in Planetary Nebulae

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