Appraising the Necklace: A post-common-envelope carbon dwarf inside an apparently carbon-poor planetary nebula

Jones, D; Corradi, RLM; Garcia Perez, GA; Morisset, C; Garcia-Rojas, J; Sabin, L; Balick, B; Wise, J; Mampaso, A; Munday, J; Rodriguez-Gil, P; del Mar Rubio-Diez, M; Santander-Garcia, M; Sowicka, P; Csukai, A; Hillwig, TC; de la Fuente, AH; Terwel, JH

Appraising the Necklace: A post-common-envelope carbon dwarf inside an apparently carbon-poor planetary nebula

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Jones, D, Corradi, RLM, Garcia Perez, GA, Morisset, C, Garcia-Rojas, J, Sabin, L, Balick, B, Wise, J ORCID: 0000-0003-0733-2916, Mampaso, A, Munday, J, Rodriguez-Gil, P, del Mar Rubio-Diez, M, Santander-Garcia, M, Sowicka, P, Csukai, A, Hillwig, TC, de la Fuente, AH and Terwel, JH (2026) Appraising the Necklace: A post-common-envelope carbon dwarf inside an apparently carbon-poor planetary nebula. Astronomy and Astrophysics, 707. ISSN 0004-6361

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Publisher URL: https://doi.org/10.1051/0004-6361/202557784

Abstract

Context: The Necklace nebula is a bipolar, post-common-envelope planetary nebula, the central star of which has been shown to have a dwarf carbon star companion.

Aims: We aim to understand the origins of the Necklace and its dwarf carbon central star.

Methods: We study the carbon abundance of the nebula through far ultraviolet spectroscopy obtained with the Hubble Space Telescope. Furthermore, through simultaneous modelling of multiband light and velocity curves, we attempt to constrain the parameters of the central star system.

Results: Puzzlingly, we find that the region of the inner nebula observed with the Hubble Space Telescope is seemingly not carbon-rich, at odds with the dwarf carbon star nature of the companion of the central star. The initial mass of the nebular progenitor was likely very close to the limit to become carbon-rich, perhaps experiencing a very late thermal pulse. The dwarf carbon star companion is found to be significantly inflated with respect to that expected for an isolated main sequence star of the same mass.

Conclusions: The properties of the central binary are consistent with the progenitor having become carbon-rich and its companion having accreted a significant amount of that carbon-enriched material. However, it is unclear how this evolutionary hypothesis can be reconciled with the inner nebula potentially being carbon poor.

Item Type:	Article
Uncontrolled Keywords:	stars: AGB and post-AGB; binaries: close; stars: chemically peculiar; white dwarfs; ISM: abundances; planetary nebulae: individual: PN G054.2-03.4; astro-ph.SR; astro-ph.SR; 5109 Space Sciences; 51 Physical Sciences; 0201 Astronomical and Space Sciences; Astronomy & Astrophysics; 5101 Astronomical sciences; 5107 Particle and high energy physics; 5109 Space sciences
Subjects:	Q Science > QB Astronomy Q Science > QC Physics
Divisions:	Astrophysics Research Institute
Publisher:	EDP Sciences
Date of acceptance:	26 January 2026
Date of first compliant Open Access:	17 March 2026
Date Deposited:	17 Mar 2026 09:55
Last Modified:	17 Mar 2026 09:55
DOI or ID number:	10.1051/0004-6361/202557784
URI:	https://researchonline.ljmu.ac.uk/id/eprint/28249

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