51. Common envelope evolution in born-again planetary nebulae – Shaping the H-deficient ejecta of A 30
- Author
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J B Rodríguez-González, E Santamaría, J A Toalá, M A Guerrero, B Montoro-Molina, G Rubio, D Tafoya, Y-H Chu, G Ramos-Larios, L Sabin, Ministerio de Ciencia e Innovación (España), European Commission, and Universidad Nacional Autónoma de México
- Subjects
Stars: evolution ,Astrophysics - Solar and Stellar Astrophysics ,Planetary nebulae: individual: PN A66 30 ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,FOS: Physical sciences ,Stars: mass-loss ,Stars: winds, outflows ,Astronomy and Astrophysics ,Circumstellar matter ,Astrophysics - Astrophysics of Galaxies ,Solar and Stellar Astrophysics (astro-ph.SR) - Abstract
Born-again planetary nebulae (PNe) are extremely rare cases in the evolution of solar-like stars. It is commonly accepted that their central stars (CSPN) experienced a very late thermal pulse (VLTP), ejecting H-deficient material inside the evolved H-rich PN. Given the short duration of this event and the fast subsequent evolution of the CSPN, details of the mass ejection are unknown. We present the first morphokinematic model of the H-deficient material surrounding a born-again PN, namely A 30. New San Pedro Mártir observations with the Manchester Echelle Spectrograph were recently obtained to map the inner region of A 30 which are interpreted by means of the software SHAPE in conjunction with HST WFC3 images. The SHAPE morphokinematic model that best reproduces the observations is composed by a disrupted disc tilted 37° with respect to the line of sight and a pair of orthogonal opposite bipolar ejections. We confirm previous suggestions that the structures closer to the CSPN present the highest expansion velocities, that is, the disrupted disc expands faster than the farther bipolar features. We propose that the current physical structure and abundance discrepancy of the H-deficient clumps around the CSPN of A 30 can be explained by a common envelope phase following the VLTP event. Our proposed scenario is also compared with other known born-again PNe (A 58, A 78, HuBi 1, and the Sakurai’s Object). © 2022 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society., JBR-G, ES, and GR acknowledge support Consejo Nacional de Ciencia y Tecnología (CONACyT, Mexico) for a student scholarship. JAT acknowledges funding from the Marcos Moshinsky Foundation (Mexico) and Dirección General de Asuntos del Personal Académico (DGAPA), Universidad Nacional Autónoma de México, through grants Programa de Apoyo a Proyectos de Investigación e Inovación Tecnológica (PAPIIT) IA101622. JAT also acknowledges support from the ‘Center of Excellence Severo Ochoa’ Visiting-Incoming program. JAT and GR-L acknowledge support from CONACyT (grant 263373). MAGR and BMM acknowledge support from the State Agency for Research of the Spanish MCIU through the ‘Center of Excellence Severo Ochoa’ award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709). Y-HC acknowledges the support of MOST grant 110-2112-M-001-020 from the Ministry of Science and Technology of Taiwan. LS acknowledges support from UNAM DGAPA PAPIIT Grant IN110122 (Mexico). This paper is based in part on ground-based observations from the Observatorio Astronómico Nacional at the Sierra de San Pedro Mártir (OAN-SPM), which is a national facility operated by the Instituto de Astronomía of the Universidad Nacional Autónoma de México. The authors thank the telescope operator P. F. Guillén for valuable guidance during several observing runs, and to the OAN-SPM staff for their valuable support. This work has made extensive use of the NASA’s Astrophysics Data System.
- Published
- 2022