Skip to content
DraconiticResearch
Search Sources API
203,234 studies31 sourcesUpdated 57 min ago
PreprintarXiv licencearXiv

Proto-Planetary Nebulae Are Not the Precursors of Planetary Nebulae With Close Binary Central Stars

  • Todd C. Hillwig
  • Bruce J. Hrivnak
  • David Jones
Open at sourcePDFDOICite

Abstract

Proto-planetary nebulae are considered to be the evolutionary link between AGB stars and planetary nebulae. They possess many of the physical characteristics expected of such a link and provide valuable information about the evolutionary process in these objects. One important characteristic of proto-planetary nebulae is the prevalence of very strong bipolar and point-symmetric morphologies. In planetary nebulae, these shapes are widely considered to be the result of shaping by a binary companion. Indeed, a number of studies have shown links between strong axial or point-symmetry in planetary nebulae and close binary central star systems that have gone through a common envelope phase. Here, we explore whether the observed proto-planetary nebulae may be the progenitors of planetary nebulae with close binary central stars. We find that despite the strong shaping of proto-planetary nebulae this is unlikely to be the case. We also discuss options for evolution to close binaries and the alternatives.

Versions

Related

  1. X-Shooter view of planetary nebulae microstructures. I. The case of NGC 7009 knots
    L. Konstantinou, S. Akras, K. Bouvis +4
    Astronomy & AstrophysicsPeer-reviewedPublisher termsSolar & stellar physicsCrossref
  2. Classification of Galactic Planetary Nebulae Among HASH Candidates
    A Demirci, Y C Atilgan, N Aksaker
    Monthly Notices of the Royal Astronomical SocietyPeer-reviewedCC BY 4.0Full textSolar & stellar physicsCrossref
  3. The jet-shaped pipe morphology in planetary nebulae and core-collapse supernova remnants
    Jessica Braudo, Noam Soker
    arXivPreprintCC BY 4.0Full textHigh-energy astrophysicsarXiv
  4. The jet-shaped pipe morphology in planetary nebulae and core-collapse supernova remnants
    Jessica Braudo, Noam Soker
    The Open Journal of AstrophysicsPeer-reviewedCC BY 4.01 citedHigh-energy astrophysicsCrossref
  5. Revealing planetary nebulae in narrow bands: a homogeneous H α imaging catalogue for morphological studies
    R A Pignata, W Weidmann, D Mast
    Monthly Notices of the Royal Astronomical SocietyPeer-reviewedCC BY 4.0Full textSolar & stellar physicsCrossref

Cite

BibTeXRIS
BibTeX
@misc{hillwig2026protoplanetary,
  title = {{Proto-Planetary Nebulae Are Not the Precursors of Planetary Nebulae With Close Binary Central Stars}},
  author = {Todd C. Hillwig and Bruce J. Hrivnak and David Jones},
  howpublished = {arXiv},
  year = {2026},
  month = sep,
  doi = {10.48550/arxiv.2609.17830},
  eprint = {2609.17830},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2609.17830},
}
RIS
TY  - UNPB
TI  - Proto-Planetary Nebulae Are Not the Precursors of Planetary Nebulae With Close Binary Central Stars
AU  - Todd C. Hillwig
AU  - Bruce J. Hrivnak
AU  - David Jones
PY  - 2026
DA  - 2026/09/15
PB  - arXiv
DO  - 10.48550/arxiv.2609.17830
UR  - https://arxiv.org/abs/2609.17830
AB  - Proto-planetary nebulae are considered to be the evolutionary link between AGB stars and planetary nebulae. They possess many of the physical characteristics expected of such a link and provide valuable information about the evolutionary process in these objects. One important characteristic of proto-planetary nebulae is the prevalence of very strong bipolar and point-symmetric morphologies. In planetary nebulae, these shapes are widely considered to be the result of shaping by a binary companion. Indeed, a number of studies have shown links between strong axial or point-symmetry in planetary nebulae and close binary central star systems that have gone through a common envelope phase. Here, we explore whether the observed proto-planetary nebulae may be the progenitors of planetary nebulae with close binary central stars. We find that despite the strong shaping of proto-planetary nebulae this is unlikely to be the case. We also discuss options for evolution to close binaries and the alternatives.
ER  -