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dc.contributor.author
Henry, R. B. C.
dc.contributor.author
Stephenson, B. G.
dc.contributor.author
Miller Bertolami, Marcelo Miguel
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dc.contributor.author
Kwitter, K. B.
dc.contributor.author
Balick, B.
dc.date.available
2019-08-29T19:13:57Z
dc.date.issued
2018-01
dc.identifier.citation
Henry, R. B. C.; Stephenson, B. G.; Miller Bertolami, Marcelo Miguel; Kwitter, K. B.; Balick, B.; On the production of He, C, and N by low- and intermediate-mass stars: A comparison of observed and model-predicted planetary nebula abundances; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 473; 1; 1-2018; 241-260
dc.identifier.issn
0035-8711
dc.identifier.uri
http://hdl.handle.net/11336/82516
dc.description.abstract
The primary goal of this paper is to make a direct comparison between the measured and model-predicted abundances of He, C, and N in a sample of 35 well-observed Galactic planetary nebulae (PNe). All observations, data reductions, and abundance determinations were performed in house to ensure maximum homogeneity. Progenitor star masses (M ≤ 4M⊙) were inferred using two published sets of post-asymptotic giant branch model tracks and L and Teff 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 ~5M⊙ 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.
dc.format
application/pdf
dc.language.iso
eng
dc.publisher
Oxford University Press
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dc.rights
info:eu-repo/semantics/openAccess
dc.rights.uri
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.subject
Galaxies: Abundances
dc.subject
Galaxies: Ism
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Ism: Abundances
dc.subject
Planetary Nebulae: General
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Stars: Agb And Post-Agb
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Stars: Evolution
dc.subject.classification
Astronomía
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dc.subject.classification
Ciencias Físicas
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dc.subject.classification
CIENCIAS NATURALES Y EXACTAS
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dc.title
On the production of He, C, and N by low- and intermediate-mass stars: A comparison of observed and model-predicted planetary nebula abundances
dc.type
info:eu-repo/semantics/article
dc.type
info:ar-repo/semantics/artículo
dc.type
info:eu-repo/semantics/publishedVersion
dc.date.updated
2019-08-28T17:58:17Z
dc.journal.volume
473
dc.journal.number
1
dc.journal.pagination
241-260
dc.journal.pais
Reino Unido
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dc.journal.ciudad
Oxford
dc.description.fil
Fil: Henry, R. B. C.. Oklahoma State University; Estados Unidos
dc.description.fil
Fil: Stephenson, B. G.. Oklahoma State University; Estados Unidos
dc.description.fil
Fil: Miller Bertolami, Marcelo Miguel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
dc.description.fil
Fil: Kwitter, K. B.. Williams College; Estados Unidos
dc.description.fil
Fil: Balick, B.. University of Washington; Estados Unidos
dc.journal.title
Monthly Notices of the Royal Astronomical Society
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dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1093/mnras/stx2286
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-abstract/473/1/241/4107117
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