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Galaxies
Special Issues
Origins and Models of Planetary Nebulae
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Origins and Models of Planetary Nebulae

A special issue of Galaxies (ISSN 2075-4434).

Deadline for manuscript submissions: 1 February 2025 | Viewed by 5281

Special Issue Editors

Dr. Andreas Ritter

E-Mail Website
Guest Editor
Laboratory for Space Research, The University of Hong Kong, Hong Kong, China
Interests: late stages of stellar evolution; astronomical spectroscopy
Prof. Dr. Xuan Fang

E-Mail Website
Guest Editor
National Astronomical Observatories, Chinese Academy of Sciences (NAOC), Beijing 100101, China
Interests: stellar evolution (in particular late-stage evolution); physics and chemistry of planetary nebulae; astronomical spectroscopy

Special Issue Information

Dear Colleagues,

We are pleased to present a Special Issue of the scientific journal Galaxies focusing on the origins and models of planetary nebulae. Planetary nebulae are fascinating astronomical objects that have captivated astronomers for centuries. They are the final stage of evolution for low-to-intermediate-mass stars, and they have been observed in a variety of shapes and sizes. The study of planetary nebulae has led to significant advancements in our understanding of stellar evolution, the interstellar medium, and the chemical enrichment of galaxies. This Special Issue brings together leading experts in the field to discuss the latest research on the origins and models of planetary nebulae. We hope that this collection of articles will provide a comprehensive overview of the current state of knowledge on this important topic and inspire further research in this exciting field.

Focus: The focus of this Special Issue is on the origins and models of planetary nebulae.

Scope: The Special Issue will cover a range of topics related to planetary nebulae, including their formation, evolution, morphology, and chemical composition. The articles will also explore the role of planetary nebulae in the enrichment of the interstellar medium and the chemical evolution of galaxies.

Purpose: The purpose of this Special Issue is to provide a comprehensive overview of the current state of knowledge on planetary nebulae and to highlight the latest research in this field. The articles will bring together leading experts in the field to discuss their findings and share new insights into the origins and models of planetary nebulae. The Special Issue aims to inspire further research in this exciting field and to deepen our understanding of the role that planetary nebulae play in the evolution of the universe.

This Special Issue will supplement existing literature by providing a focused and in-depth exploration of the origins and models of planetary nebulae. While there have been numerous studies on planetary nebulae, this collection of articles will bring together the latest research and findings in a consolidated manner. By featuring contributions from leading experts in the field, the Special Issue will offer new perspectives and insights that build and expand upon the existing literature. The articles included in this Special Issue will delve into specific aspects of planetary nebulae, such as their formation mechanisms, evolutionary processes, and diverse morphologies. They will also explore the chemical composition of planetary nebulae and their role in the chemical enrichment of the interstellar medium and galaxies. By presenting a comprehensive overview of the current state of knowledge, the Special Issue will help to consolidate and synthesize existing research, while also highlighting any gaps or areas for future investigation. Furthermore, the Special Issue will not only present new findings but also provide critical analyses and discussions of existing models and theories. This will allow readers to critically evaluate and compare different approaches and interpretations, contributing to a deeper understanding of the origins and models of planetary nebulae. Overall, the Special Issue will serve as a valuable resource for researchers, students, and enthusiasts interested in this fascinating field, further enriching and supplementing the existing literature.

Dr. Andreas Ritter
Prof. Dr. Xuan Fang
Guest Editors

Manuscript Submission Information

Manuscripts should be submitted online at www.mdpi.com by registering and logging in to this website. Once you are registered, click here to go to the submission form. Manuscripts can be submitted until the deadline. All submissions that pass pre-check are peer-reviewed. Accepted papers will be published continuously in the journal (as soon as accepted) and will be listed together on the special issue website. Research articles, review articles as well as short communications are invited. For planned papers, a title and short abstract (about 100 words) can be sent to the Editorial Office for announcement on this website.

Submitted manuscripts should not have been published previously, nor be under consideration for publication elsewhere (except conference proceedings papers). All manuscripts are thoroughly refereed through a single-blind peer-review process. A guide for authors and other relevant information for submission of manuscripts is available on the Instructions for Authors page. Galaxies is an international peer-reviewed open access semimonthly journal published by MDPI.

Please visit the Instructions for Authors page before submitting a manuscript. The Article Processing Charge (APC) for publication in this open access journal is 1400 CHF (Swiss Francs). Submitted papers should be well formatted and use good English. Authors may use MDPI's English editing service prior to publication or during author revisions.

Keywords

  • planetary nebulae
  • nebulae around massive stars
  • nova remnants
  • symbiotic stars
  • shaping mechanisms
  • binary stars

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Published Papers (5 papers)

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Research

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9 pages, 7780 KiB  
Article
On the Ionization Tolerance of C20 Fullerene in Ground and Excited Electronic States in Planetary Nebulae
by SeyedAbdolreza Sadjadi and Quentin Andrew Parker
Galaxies 2024, 12(6), 84; https://doi.org/10.3390/galaxies12060084 - 30 Nov 2024
Viewed by 322
Abstract
As the smallest member of the fullerene family, C20 is yet to be discovered in planetary nebulae. In this work, we present a quantum chemical study via density functional theory (DFT) and partially by the MP2 on the ionization tolerance of this [...] Read more.
As the smallest member of the fullerene family, C20 is yet to be discovered in planetary nebulae. In this work, we present a quantum chemical study via density functional theory (DFT) and partially by the MP2 on the ionization tolerance of this molecule in the space environment. Considering that the ionization and excitation phenomena play key roles in demonstrating the lifetime of a molecule, we examined both ground and excited electronic-state potential energy surfaces (PES) of C20 and its cations C20q+. Our theoretical results indicate that the C20 cage tolerates a positive charge as high as 13+ by characterizing local minimum geometries on both the abovementioned electronic states. The results are backed by characterizing both C2012+ and C2013+ as local minimum geometries at the MP2 level of computations. We also explored, theoretically and systematically, scenarios in which the electronic structure of neutral C20 is excited to very high spin multiplicity (beyond triplet state), and local minimum molecular geometries with cage structures are well characterized. We anticipate that such structural resistance to excitation and ionization delivers a prolonged lifetime necessary for the spectroscopic detection of this interesting molecule and its cations in space and potentially in planetary nebulae (PN). Full article
(This article belongs to the Special Issue Origins and Models of Planetary Nebulae)
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21 pages, 2057 KiB  
Article
A Dust-Scattering Model for M1-92: A Revised Estimate of the Mass Distribution and Inclination
by Yun Qi Li, Mark R. Morris and Raghvendra Sahai
Galaxies 2024, 12(4), 44; https://doi.org/10.3390/galaxies12040044 - 5 Aug 2024
Viewed by 858
Abstract
Preplanetary nebulae (PPNe) are formed from mass-ejecting late-stage AGB stars. Much of the light from the star gets scattered or absorbed by dust particles, giving rise to the observed reflection nebula seen at visible and near-IR wavelengths. Precursors to planetary nebulae (PNe), PPNe [...] Read more.
Preplanetary nebulae (PPNe) are formed from mass-ejecting late-stage AGB stars. Much of the light from the star gets scattered or absorbed by dust particles, giving rise to the observed reflection nebula seen at visible and near-IR wavelengths. Precursors to planetary nebulae (PNe), PPNe generally have not yet undergone any ionization by UV radiation from the still-buried stellar core. Bipolar PPNe are a common form of observed PPNe. This study lays the groundwork for future dynamical studies by reconstructing the dust density distribution of a particularly symmetric bipolar PPN, M1-92 (Minkowski’s Footprint, IRAS 19343+2926). For this purpose, we develop an efficient single-scattering radiative transfer model with corrections for double-scattering. Using a V-band image from the Hubble Space Telescope (HST), we infer the dust density profile and orientation of M1-92. These results indicate that M1-92’s slowly expanding equatorial torus exhibits an outer radial cutoff in its density, which implicates the influence of a binary companion during the formation of the nebula. Full article
(This article belongs to the Special Issue Origins and Models of Planetary Nebulae)
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14 pages, 7277 KiB  
Article
Planetary Nebula Morphologies Indicate a Jet-Driven Explosion of SN 1987A and Other Core-Collapse Supernovae
by Noam Soker
Galaxies 2024, 12(3), 29; https://doi.org/10.3390/galaxies12030029 - 6 Jun 2024
Cited by 5 | Viewed by 823
Abstract
I demonstrate the usage of planetary nebulae (PNe) to infer that a pair of jets shaped the ejecta of the core-collapse supernova (CCSN) SN 1987A. The main structure of the SN 1987A inner ejecta, the ‘keyhole’, comprises two low-intensity zones. The northern one [...] Read more.
I demonstrate the usage of planetary nebulae (PNe) to infer that a pair of jets shaped the ejecta of the core-collapse supernova (CCSN) SN 1987A. The main structure of the SN 1987A inner ejecta, the ‘keyhole’, comprises two low-intensity zones. The northern one has a bright rim on its front, while the southern one has an elongated nozzle. An earlier comparison of the SN 1987A ‘keyhole’ with bubbles in the galaxy group NGC 5813 led to its identification as a jet-shaped rim–nozzle structure. Here, I present rim–nozzle asymmetry in planetary nebulae (PNe), thought to be shaped by jets, which solidifies the claim that jets powered the ejecta of SN 1987A and other CCSNe. This finding for the iconic SN 1987A with its unique properties strengthens the jittering-jets explosion mechanism (JJEM) of CCSNe. In a few hundred years, the CCSN 1987A will have a complicated structure with two main symmetry axes, one along the axis of the three circumstellar rings that was shaped by two opposite 20,000-year pre-explosion jets, and the other along the long axis of the ‘keyhole’ that was shaped by the main (but not the only) jet pair of the exploding jets of SN 1987A in the frame of the JJEM. Full article
(This article belongs to the Special Issue Origins and Models of Planetary Nebulae)
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Review

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32 pages, 3308 KiB  
Review
Primer on Formation and Evolution of Hydrogen-Deficient Central Stars of Planetary Nebulæ and Related Objects
by Marcelo M. Miller Bertolami
Galaxies 2024, 12(6), 83; https://doi.org/10.3390/galaxies12060083 - 29 Nov 2024
Viewed by 327
Abstract
We present a brief review of the formation and evolution of hydrogen-deficient central stars of planetary nebulae. We include a detailed description of the main observable features of both the central stars and their surrounding nebulae and review their main classifications. We also [...] Read more.
We present a brief review of the formation and evolution of hydrogen-deficient central stars of planetary nebulae. We include a detailed description of the main observable features of both the central stars and their surrounding nebulae and review their main classifications. We also provide a brief description of the possible progenitor systems of hydrogen-deficient central stars as well as of transients, which are closely connected to the formation of these stars. In particular, we offer a detailed theoretical explanation of the main evolutionary scenarios, both single and binary, which is devised to explain these stars and nebulae. Particular emphasis is made in the description of the so-called born again scenario, their quantitative predictions, and uncertainties. Finally, we discuss the pros and cons of both binary and single evolution channels, draw some conclusions, and discuss open questions in the field. Full article
(This article belongs to the Special Issue Origins and Models of Planetary Nebulae)
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19 pages, 5710 KiB  
Review
Planetary Nebulae Research: Past, Present, and Future
by Sun Kwok
Galaxies 2024, 12(4), 39; https://doi.org/10.3390/galaxies12040039 - 17 Jul 2024
Cited by 1 | Viewed by 1884
Abstract
We review the evolution of our understanding of the planetary nebulae phenomenon and their place in the scheme of stellar evolution. The historical steps leading to our current understanding of central star evolution and nebular formation are discussed. Recent optical imaging, X-ray, ultraviolet, [...] Read more.
We review the evolution of our understanding of the planetary nebulae phenomenon and their place in the scheme of stellar evolution. The historical steps leading to our current understanding of central star evolution and nebular formation are discussed. Recent optical imaging, X-ray, ultraviolet, infrared, millimeter wave, and radio observations have led to a much more complex picture of the structure of planetary nebulae. The optically bright regions have multiple shell structures (rims, shells, crowns, and haloes), which can be understood within the interacting winds framework. However, the physical mechanism responsible for bipolar and multipolar structures that emerged during the proto-planetary nebulae phase is yet to be identified. Our morphological classifications of planetary nebulae are hampered by the effects of sensitivity, orientation, and field-of-view coverage, and the fraction of bipolar or multipolar nebulae may be much higher than commonly assumed. The optically bright bipolar lobes may represent low-density, ionization-bounded cavities carved out of a neutral envelope by collimated fast winds. Planetary nebulae are sites of active synthesis of complex organic compounds, suggesting that planetary nebulae play a major role in the chemical enrichment of the Galaxy. Possible avenues of future advancement are discussed. Full article
(This article belongs to the Special Issue Origins and Models of Planetary Nebulae)
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