CO-SPATIAL LONG-SLIT UV/OPTICAL SPECTRA OF TEN GALACTIC PLANETARY NEBULAE WITH<i>HST</i>/STIS. II. NEBULAR MODELS, CENTRAL STAR PROPERTIES, AND He+CNO SYNTHESIS

Henry, R. B. C.; Balick, Bruce; Dufour, R. J.; Kwitter, K. B.; Shaw, Richard A.; Miller, Timothy R.; Buell, J. F.; Corradi, R. L. M.

doi:10.1088/0004-637x/813/2/121

Cited by 13 publications

(16 citation statements)

References 52 publications

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“…1, the surface carbon (7.37) is too small for this interpretation (but note the huge errorbar). Note that the carbon abundance whose derivation is based on photoionisation models C/H = 8.13 (Henry et al 2015) is in much better agreement with our interpretation. NGC 7662 is a inhomogeneous PN, with a lot of stratification (see Dufour et al 2015).…”

Section: Dddm 1 (Pn G0619+413)supporting

confidence: 87%

“…We also searched the literature for Galactic PNe whose spectra has been acquired with the HST. Henry et al (2015) and Dufour et al (2015) examined 7 carbon determinations in Galactic PNe (4 in common with the IUE samples described above). Furthermore, Henry et al (2008) observed the halo PN DdDm 1 (PN G061.9+41.3), and Bianchi et al (2001) observed a globular cluster PN (K648 in M15).…”

Section: Sample 1 Pnementioning

confidence: 99%

“…We comment on possible use of the model abundances from Henry et al (2015), based on Dufour et al' s (2015) data, in specific cases in the following sections. It is important to note that we have checked all PNe in this sample for possibly being located in the bulge or halo of the Galaxy, according to the definition which is commonly adopted (see Stanghellini & Haywood 2010).…”

Section: Sample 1 Pnementioning

confidence: 99%

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The evolution of Galactic planetary nebula progenitors through the comparison of their nebular abundances with AGB yields

Ventura

Stanghellini

Dell’Agli

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We study the chemical abundances of a wide sample of 142 Galactic planetary nebulae (PNe) with good quality observations, for which the abundances have been derived more or less homogeneously, thus allowing a reasonable comparison with stellar models. The goal is the determination of mass, chemical composition and formation epoch of their progenitors, through comparison of the data with results from AGB evolution. The dust properties of PNe, when available, were also used to further support our interpretation.We find that the majority (∼ 60%) of the Galactic PNe studied has nearly solar chemical composition, while ∼ 40% of the sources investigated have sub-solar metallicities. About half of the PNe have carbon star progenitors, in the 1.5 M ⊙ < M < 3 M ⊙ mass range, which have formed between 300 Myr and 2 Gyr ago. The remaining PNe are almost equally distributed among PNe enriched in nitrogen, which we interpret as the progeny of M > 3.5 M ⊙ stars, younger than 250 Myr, and a group of oxygen-rich PNe, descending from old (> 2 Gyr) low-mass (M < 1.5 M ⊙ ) stars that never became C-stars.This analysis confirms the existence of an upper limit to the amount of carbon which can be accumulated at the surface of carbon stars, probably due to the acceleration of mass loss in the late AGB phases. The chemical composition of the present sample suggests that in massive AGB stars of solar (or slightly sub-solar) metallicity, the effects of third dredge up combine with hot bottom burning, resulting in nitrogenrich -but not severely carbon depleted -gaseous material to be ejected.

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Section: Dddm 1 (Pn G0619+413)supporting

confidence: 87%

Section: Sample 1 Pnementioning

confidence: 99%

Section: Sample 1 Pnementioning

confidence: 99%

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The evolution of Galactic planetary nebula progenitors through the comparison of their nebular abundances with AGB yields

Ventura

Stanghellini

Dell’Agli

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…The values of log(L/L ⊙ ) and log T ef f were taken from Frew (2008) for 32 of our 35 sample objects. For the three sample objects not included in Frew (2008) (IC2165, IC3568 and NGC5315) we assumed the L and T values derived from models in Henry et al (2015).…”

Section: Progenitor Star Massesmentioning

confidence: 99%

“…9.8 of Frew (2008), since uncertainties for individual objects were not provided. Because each track is associated with a specific initial and final mass, we carefully measured each object's displacement from adjacent Tables 5 and 6 in Henry et al (2015) were assumed.…”

Section: Progenitor Star Massesmentioning

confidence: 99%

On the production of He, C, and N by low- and intermediate-mass stars: a comparison of observed and model-predicted planetary nebula abundances

Henry

Stephenson

Bertolami

et al. 2017

Monthly Notices of the Royal Astronomical Society

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The primary goal of this paper is to make a direct comparison between the measured and modelpredicted abundances of He, C and N in a sample of 35 well-observed Galactic planetary nebulae (PN). All observations, data reductions, and abundance determinations were performed in house to ensure maximum homogeneity. Progenitor star masses (M ≤ 4 M ⊙ ) were inferred using two published sets of post-AGB model tracks and L and T ef f values. We conclude the following: 1) the mean values of N/O across the progenitor mass range exceeds the solar value, indicating significant N enrichment in the majority of our objects; 2) the onset of hot bottom burning appears to begin around 2 M ⊙ , i.e., lower than ∼ 5 M ⊙ implied by theory; 3) most of our objects show a clear He enrichment, as expected from dredge-up episodes; 4) the average sample C/O value is 1.23, consistent with the effects of third dredge-up; and 5) model grids used to compare to observations successfully span the distribution over metallicity space of all C/O and many He/H data points but mostly fail to do so in the case of N/O. The evident enrichment of N in PN and the general discrepancy between the observed and model-predicted N/O abundance ratios signal the need for extra-mixing as an effect of rotation and/or thermohaline mixing in the models. The unexpectedly high N enrichment that is implied here for low mass stars, if confirmed, will likely impact our conclusions about the source of N in the Universe.

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IFU Spectroscopy of Southern Planetary Nebulae V: Low-Ionisation Structures

Ali

Dopita

2017

Publ. Astron. Soc. Aust.

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In this 5th paper of the series, we examine the spectroscopy and morphology of four southern Galactic planetary nebulae Hen 2-141, NGC 5307, IC 2553, and PB 6 using new integral field spectroscopy data. The morphologies and ionization structures of the sample are given as a set of emission-line maps. In addition, the physical conditions, chemical compositions, and kinematical characteristics of these objects are derived. The results show that PB 6 and Hen 2-141 are of very high excitation classes and IC 2553 and NGC 5307 are mid to high excitation objects. The elemental abundances reveal that PB 6 is of Type I, Hen 2-141 and IC 2553 are of Type IIa, and NGC 5307 of Type IIb/III. The observations unveil the presence of welldefined low-ionization structures or "knots" in all objects. The diagnostic diagrams reveal that the excitation mechanism of these knots is probably by photo-ionization of dense material by the nebular central stars. The physical analysis of six of these knots show no significant differences with their surrounding nebular gas, except their lower electron densities. In spite of the enhancement of the low-ionization emission lines of these knots, their chemical abundances are nearly comparable to their surrounding nebulae, with the exception of perhaps slightly higher nitrogen abundances in the NGC 5307 knots. The integrated spectrum of IC 2553 reveals that nearly all key lines that have led researchers to characterize its central star as a weak-emission line star type are in fact of nebular origin.

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CO-SPATIAL LONG-SLIT UV/OPTICAL SPECTRA OF TEN GALACTIC PLANETARY NEBULAE WITHHST/STIS. II. NEBULAR MODELS, CENTRAL STAR PROPERTIES, AND He+CNO SYNTHESIS

Cited by 13 publications

References 52 publications

The evolution of Galactic planetary nebula progenitors through the comparison of their nebular abundances with AGB yields

The evolution of Galactic planetary nebula progenitors through the comparison of their nebular abundances with AGB yields

On the production of He, C, and N by low- and intermediate-mass stars: a comparison of observed and model-predicted planetary nebula abundances

IFU Spectroscopy of Southern Planetary Nebulae V: Low-Ionisation Structures

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