Hostname: page-component-cd9895bd7-q99xh Total loading time: 0 Render date: 2024-12-25T06:03:30.788Z Has data issue: false hasContentIssue false
  • English
  • Français

Understanding Galactic planetary nebulae with precise/reliable nebular abundances

Published online by Cambridge University Press:  08 August 2017

D. A. García-Hernández ,
P. Ventura ,
G. Delgado-Inglada ,
F. Dell'Agli ,
M. Di Criscienzo  and
A. Yagüe
D. A. García-Hernández
Affiliation:
Instituto de Astrofísica de Canarias, C/ Vía Láctea s/n, E−38205 La Laguna, Spain Departamento de Astrofísica, Universidad de La Laguna, E−38206 La Laguna, Spain
P. Ventura
Affiliation:
INAF - OAR, Via Frascati 33, 00040, Monte Porzio Catone, Italy
G. Delgado-Inglada
Affiliation:
Instituto de Astronomía, UNAM, Apdo. Postal 70264, 04510, México D. F., México
F. Dell'Agli
Affiliation:
Instituto de Astrofísica de Canarias, C/ Vía Láctea s/n, E−38205 La Laguna, Spain Departamento de Astrofísica, Universidad de La Laguna, E−38206 La Laguna, Spain INAF - OAR, Via Frascati 33, 00040, Monte Porzio Catone, Italy
M. Di Criscienzo
Affiliation:
INAF - OAR, Via Frascati 33, 00040, Monte Porzio Catone, Italy
A. Yagüe
Affiliation:
Instituto de Astrofísica de Canarias, C/ Vía Láctea s/n, E−38205 La Laguna, Spain Departamento de Astrofísica, Universidad de La Laguna, E−38206 La Laguna, Spain INAF - OAR, Via Frascati 33, 00040, Monte Porzio Catone, Italy
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We compare recent precise/reliable nebular abundances - as derived from high-quality optical spectra and the most recent ICFs - in a sample of Galactic planetary nebulae (PNe) with nucleosynthesis predictions (HeCNOCl) from asymptotic giant branch (AGB) ATON models in the metallicity range Z⊙/4 < Z < 2Z⊙. According to the infrared dust features, the sample is divided among carbon-, oxygen-, and double-dust chemistry (CC, OC, and DC, respectively), providing an independent proxy for the nature of the PNe progenitors. Our AGB models, with diffusive overshooting from all the convective borders, nicely reproduce the O overabundances observed in CC PNe, indicating that they evolve from low-Z low-mass (∼1 −3 M⊙) AGB stars. This indicates that O is not always a good indicator of the original ISM metallicity and that the O production by low-mass stars should be considered in galactic-evolution models. The lowest metallicity OC PNe evolve from low-mass (∼1 M⊙) O-rich AGBs, while the higher metallicity ones (all with uncertain dust classifications) display a chemical pattern similar to the DC PNe. In agreement with the recent literature, the DC PNe mostly descend from high-mass (M > 3.5 M⊙) solar/supersolar metallicity AGBs that experience hot bottom burning (HBB), but other formation channels in low-mass AGBs like extra mixing, stellar rotation, binary interaction, or He pre-enrichment cannot be disregarded until more accurate C/O ratios can be obtained. Two DC PNe show the imprint of advanced CNO processing and deep second dredge-up, suggesting progenitors masses close to the limit to evolve as core collapse supernovae (above 6 M⊙). Their actual C/O ratios, if confirmed, indicate contamination from the third dredge-up, rejecting the hypothesis that the chemical composition of such high-metallicity massive AGBs is modified exclusively by HBB.

Keywords

Nuclear reactionsnucleosynthesisabundancesISM: abundancesH II regionsplanetary nebulae: generalGalaxy: abundances
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S323: Planetary Nebulae: Multi-Wavelength Probes of Stellar and Galactic Evolution , October 2016 , pp. 95 - 98
Copyright
Copyright © International Astronomical Union 2017 

References

Delgado-Inglada, G., Rodríguez, M., Peimbert, M., et al. 2015, MNRAS, 449, 1797 Google Scholar
García-Hernández, D. A., Ventura, P., Delgado-Inglada, G., et al. 2016a, MNRAS, 458, L118 CrossRefGoogle Scholar
García-Hernández, D. A., Ventura, P., Delgado-Inglada, G., et al. 2016b, MNRAS, 461, 542 Google Scholar
Herwig, F., Blöcker, T., Schönberner, D., El Eid, M., 1997, A&A, 324, L81 Google Scholar
Karakas, A. I., 2010, MNRAS, 403, 1413 Google Scholar
Karakas, A. I., Lattanzio, J. C., 2014, PASA, 31, 30 Google Scholar
Marigo, P. & Aringer B., 2009, A&A, 508, 1538 Google Scholar
Pignatari, M., Herwig, F., Hirschi, R., et al. 2016, ApJS, 225, 24 Google Scholar
Ventura, P., Stanghellini, L., Dell’Agli, F., et al. 2015, MNRAS, 452, 3679 Google Scholar
Richer, M. G. 2015, in IAU General Assembly, Meeting #29, #2256079Google Scholar