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Peer-reviewedCC BY 4.0Monthly Notices of the Royal Astronomical Society

A morpho-kinematic view of the Necklace nebula

  • E Santamaría1,2
  • J A Toalá1
  • L Sabin3
  • M A Guerrero4
  • G Ramos-Larios2
4 affiliations
  1. 1Instituto de Radioastronomía y Astrofísica , Universidad Nacional Autónoma de México, Morelia 58089, Michoacán ,
  2. 2Instituto de Astronomía y Meteorología , Dpto. de Física, CUCEI, Universidad de Guadalajara, Guadalajara, Jalisco ,
  3. 3Instituto de Astronomía, Universidad Nacional Autónoma de México , AP 106, Ensenada 22800, BC ,
  4. 4Instituto de Astrofísica de Andalucía , CSIC, Glorieta de la Astronomía S/N, Granada 18008 ,
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Abstract

We present a morpho-kinematic study of the Necklace Nebula based on spatially resolved spectroscopic observations and 3D modeling performed with the shape software. The nebula is characterized by an equatorial disrupted ring accompanied by bipolar outflows. The geometry and velocity field of these different components are derived from the comparison between observed and synthetic images and position-velocity diagrams. The best model successfully reproduces the main morphological and kinematic features of the nebula, allowing us to constrain its 3D structure. We confirm that the disrupted ring is tilted about 60○ from the plane of the sky, but the bipolar outflows are inclined by 46○ with respect to the line of sight. This situation might indicate that the bipolar structures are not simple extensions of the equatorial ring, but instead correspond to a distinct mass-ejection event. The slight misalignment between these two components suggests either precession of the ejection axis, a temporal change in the dominant mass-loss geometry, or a misalignment in the magnetic field. Given that the Necklace Nebula hosts a close binary central star and is a well-established post-common envelope planetary nebula, our results support a scenario in which binary interaction plays a central role in shaping its morphology, even before the common envelope phase.

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Cite

BibTeXRIS
BibTeX
@article{santamaria2026morphokinematic,
  title = {{A morpho-kinematic view of the Necklace nebula}},
  author = {E Santamaría and J A Toalá and L Sabin and M A Guerrero and G Ramos-Larios},
  journal = {Monthly Notices of the Royal Astronomical Society},
  year = {2026},
  month = oct,
  doi = {10.1093/mnras/stag2030},
  url = {https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/stag2030/8997910},
  note = {CC BY 4.0},
}
RIS
TY  - JOUR
TI  - A morpho-kinematic view of the Necklace nebula
AU  - E Santamaría
AU  - J A Toalá
AU  - L Sabin
AU  - M A Guerrero
AU  - G Ramos-Larios
PY  - 2026
DA  - 2026/10/24
JO  - Monthly Notices of the Royal Astronomical Society
DO  - 10.1093/mnras/stag2030
UR  - https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/stag2030/8997910
AB  - We present a morpho-kinematic study of the Necklace Nebula based on spatially resolved spectroscopic observations and 3D modeling performed with the shape software. The nebula is characterized by an equatorial disrupted ring accompanied by bipolar outflows. The geometry and velocity field of these different components are derived from the comparison between observed and synthetic images and position-velocity diagrams. The best model successfully reproduces the main morphological and kinematic features of the nebula, allowing us to constrain its 3D structure. We confirm that the disrupted ring is tilted about 60○ from the plane of the sky, but the bipolar outflows are inclined by 46○ with respect to the line of sight. This situation might indicate that the bipolar structures are not simple extensions of the equatorial ring, but instead correspond to a distinct mass-ejection event. The slight misalignment between these two components suggests either precession of the ejection axis, a temporal change in the dominant mass-loss geometry, or a misalignment in the magnetic field. Given that the Necklace Nebula hosts a close binary central star and is a well-established post-common envelope planetary nebula, our results support a scenario in which binary interaction plays a central role in shaping its morphology, even before the common envelope phase.
SN  - 0035-8711
SN  - 1365-2966
ER  -