TY - JOUR
T1 - Common envelope evolution in born-again planetary nebulae - Shaping the H-deficient ejecta of A 30
AU - Rodríguez-González, J. B.
AU - Santamaría, E.
AU - Toalá, J. A.
AU - Guerrero, A. A.
AU - Montoro-Molina, B.
AU - Rubio, G.
AU - Tafoya, D.
AU - Chu, Y. H.
AU - Ramos-Larios, G.
AU - Sabin, L.
N1 - Publisher Copyright:
© 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.
PY - 2022/8/1
Y1 - 2022/8/1
N2 - 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).
AB - 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).
KW - circumstellar matter
KW - planetary nebulae: individual: PN A66 30
KW - stars: evolution
KW - stars: mass-loss
KW - stars: winds, outflows
UR - http://www.scopus.com/inward/record.url?scp=85134386711&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85134386711&partnerID=8YFLogxK
U2 - 10.1093/mnras/stac1697
DO - 10.1093/mnras/stac1697
M3 - Article
AN - SCOPUS:85134386711
SN - 0035-8711
VL - 514
SP - 4794
EP - 4802
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 4
ER -