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

Formation and Evolution of [Wolf-Rayet] Planetary Nebulae through a Late Thermal Pulse

  • J B Rodríguez-González1,2
  • R Orozco-Duarte1
  • J A Toalá1
  • M M Miller Bertolami3,4
  • H Todt5
  • M A Guerrero2
  • L Conmy6
  • R Kuiper6
6 affiliations
  1. 1Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México , 58089 Morelia, Michoacán ,
  2. 2Instituto de Astrofísica de Andalucía , IAA-CSIC, Glorieta de la Astronomía S/N, Granada 18008 ,
  3. 3Instituto de Astrofísica de La Plata, Consejo Nacional de Investigaciones Científicas y Técnicas , Avenida Centenario S/N, La Plata B1900FWA ,
  4. 4Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Avenida Centenario S/N , La Plata B1900FWA ,
  5. 5Institut für Physik und Astronomie, Universität Potsdam , Karl-Liebknecht-Straße 24/25, D-14476 Potsdam ,
  6. 6Fakultät für Physik, Universität Duisburg-Essen , Lotharstraße 1, D-47057 Duisburg ,
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Abstract

We present radiation-hydrodynamical simulations of the formation of a born-again planetary nebula (PN) triggered by a late thermal pulse (LTP). The 2D radiation-hydrodynamic simulations, performed with the pluto code, follow the stellar and wind properties resulted from a stellar evolution model calculated with the Modules for Experiments in Stellar Astrophysics (mesa) code. This mesa model uses a mass-loss prescription tailored for H-deficient [Wolf-Rayet]([WR])-type winds during the post-LTP phase. Our stellar model reproduces the nearly complete depletion of H expected after an LTP event, while matching the observed abundances and spectral types of iconic [WR]-type central stars of PNe. The simulations show that the H-deficient LTP ejecta forms a transient double-shell structure which, after ~1000 yr, becomes fully mixed with the H-rich PN. The H-deficient ejecta mass (2.9 × 10−6 M⊙) is too small compared to the H-rich nebular mass of ~1.1 M⊙ ejected during the last phases of stellar evolution to leave a lasting imprint on the nebular abundances, predicting an H-rich PNe around a [WR] central star. The injection of LTP material into the PN drives turbulence, clump formation, and enhanced mixing, providing an explanation to the larger expansion velocities and larger turbulent nebular structures of PNe with [WR] central stars compared to those with H-rich central stars. These results provide robust support for the born-again scenario as the origin of H-deficient [WR] central stars within H-rich PNe.

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Cite

BibTeXRIS
BibTeX
@article{rodriguezgonzalez2026formation,
  title = {{Formation and Evolution of [Wolf-Rayet] Planetary Nebulae through a Late Thermal Pulse}},
  author = {J B Rodríguez-González and R Orozco-Duarte and J A Toalá and M M Miller Bertolami and H Todt and M A Guerrero and L Conmy and R Kuiper},
  journal = {Monthly Notices of the Royal Astronomical Society},
  year = {2026},
  month = nov,
  doi = {10.1093/mnras/stag2011},
  url = {https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/stag2011/9017893},
  note = {CC BY 4.0},
}
RIS
TY  - JOUR
TI  - Formation and Evolution of [Wolf-Rayet] Planetary Nebulae through a Late Thermal Pulse
AU  - J B Rodríguez-González
AU  - R Orozco-Duarte
AU  - J A Toalá
AU  - M M Miller Bertolami
AU  - H Todt
AU  - M A Guerrero
AU  - L Conmy
AU  - R Kuiper
PY  - 2026
DA  - 2026/11/06
JO  - Monthly Notices of the Royal Astronomical Society
DO  - 10.1093/mnras/stag2011
UR  - https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/stag2011/9017893
AB  - We present radiation-hydrodynamical simulations of the formation of a born-again planetary nebula (PN) triggered by a late thermal pulse (LTP). The 2D radiation-hydrodynamic simulations, performed with the pluto code, follow the stellar and wind properties resulted from a stellar evolution model calculated with the Modules for Experiments in Stellar Astrophysics (mesa) code. This mesa model uses a mass-loss prescription tailored for H-deficient [Wolf-Rayet]([WR])-type winds during the post-LTP phase. Our stellar model reproduces the nearly complete depletion of H expected after an LTP event, while matching the observed abundances and spectral types of iconic [WR]-type central stars of PNe. The simulations show that the H-deficient LTP ejecta forms a transient double-shell structure which, after ~1000 yr, becomes fully mixed with the H-rich PN. The H-deficient ejecta mass (2.9 × 10−6 M⊙) is too small compared to the H-rich nebular mass of ~1.1 M⊙ ejected during the last phases of stellar evolution to leave a lasting imprint on the nebular abundances, predicting an H-rich PNe around a [WR] central star. The injection of LTP material into the PN drives turbulence, clump formation, and enhanced mixing, providing an explanation to the larger expansion velocities and larger turbulent nebular structures of PNe with [WR] central stars compared to those with H-rich central stars. These results provide robust support for the born-again scenario as the origin of H-deficient [WR] central stars within H-rich PNe.
SN  - 0035-8711
SN  - 1365-2966
ER  -