Physical Conditions and Chemical Abundances in Photoionized Nebulae from Optical Spectra

García‐Rojas, J.

doi:10.1007/978-3-030-38509-5_4

Cited by 4 publications

(3 citation statements)

References 142 publications

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“…Several good review papers have been published recently addressing the subjects of nebular physics and abundance determinations from recombination and collisionally excited lines. 6 Readers who are unfamiliar with these topics or who desire a refresher course are referred to articles by Kwitter & Henry (2011), Pérez-Montero (2017), Peimbert et al (2017), Peimbert (2019), andGarcía-Rojas (2020).…”

Section: Chemical Abundances In Planetary Nebulaementioning

confidence: 99%

“…We also discuss the molecular and dust components of PNe. The extensive nebular astrophysics involved in calculating these abundances is not included here, but is comprehensively discussed in excellent recent reviews by Peimbert et al (2017) and García-Rojas (2020). Then in Section 4 we discuss radial abundance gradients in galaxy disks, and go on to compare observed abundances with theoretical predictions.…”

Section: Introductionmentioning

confidence: 99%

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Planetary Nebulae: Sources of Enlightenment

Kwitter

Henry

2022

PASP

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In this review/tutorial we explore planetary nebulae as a stage in the evolution of low-to-intermediate-mass stars, as major contributors to the mass and chemical enrichment of the interstellar medium, and as astrophysical laboratories. We discuss many observed properties of planetary nebulae, placing particular emphasis on element abundance determinations and comparisons with theoretical predictions. Dust and molecules associated with planetary nebulae are considered as well. We then examine distances, binarity, and planetary nebula morphology and evolution. We end with mention of some of the advances that will be enabled by future observing capabilities.

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Section: Chemical Abundances In Planetary Nebulaementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Planetary Nebulae: Sources of Enlightenment

Kwitter

Henry

2022

PASP

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“…Abundances of H II regions and planetary nebulae are excellent probes of the radial abundance gradient of the Milky Way (e.g., Esteban et al, 2017Arellano-Córdova et al, 2020;Stanghellini et al, 2020). For a discussion on the methods and on the challenging issues on nebular abundances, we refer to Kewley et al (2019) and García-Rojas (2020). In addition, the recent review of Maiolino and Mannucci (2019) summarizes the use of N/O and C/O abundance ratios as tracers of the evolution of the Milky Way and of nearby galaxies.…”

Section: The Galactic Evolution Of Cnomentioning

confidence: 99%

Light Elements in the Universe

Randich

Magrini

2021

Front. Astron. Space Sci.

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Due to their production sites, as well as to how they are processed and destroyed in stars, the light elements are excellent tools to investigate a number of crucial issues in modern astrophysics: from stellar structure and non-standard processes at work in stellar interiors to age dating of stars; from pre-main sequence evolution to the star formation histories of young clusters and associations and to multiple populations in globular clusters; from Big Bang nucleosynthesis to the formation and chemical enrichment history of the Milky Way Galaxy and its populations, just to cite some relevant examples. In this paper, we focus on lithium, beryllium, and boron (LiBeB) and on carbon, nitrogen, and oxygen (CNO). LiBeB are rare elements, with negligible abundances with respect to hydrogen; on the contrary, CNO are among the most abundant elements in the Universe, after H and He. Pioneering observations of light-element surface abundances in stars started almost 70 years ago and huge progress has been achieved since then. Indeed, for different reasons, precise measurements of LiBeB and CNO are difficult, even in our Sun; however, the advent of state-of-the-art ground- and space-based instrumentation has allowed the determination of high-quality abundances in stars of different type, belonging to different Galactic populations, from metal-poor halo stars to young stars in the solar vicinity and from massive stars to cool dwarfs and giants. Noticeably, the recent large spectroscopic surveys performed with multifiber spectrographs have yielded detailed and homogeneous information on the abundances of Li and CNO for statistically significant samples of stars; this has allowed us to obtain new results and insights and, at the same time, raise new questions and challenges. A complete understanding of the light-element patterns and evolution in the Universe has not been still achieved. Perspectives for further progress will open up soon thanks to the new generation instrumentation that is under development and will come online in the coming years.

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