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Akras, S,Clyne, N,Boumis, P,Monteiro, H,Goncalves, DR,Redman, MP,Williams, S
2016
April
Monthly Notices Of The Royal Astronomical Society
Deciphering the bipolar planetary nebula Abell 14 with 3D ionization and morphological studies
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Altmetric: 2WOS: 11 ()
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binaries: general ISM: abundances ISM: kinematics and dynamics planetary nebulae: individual: Abell 14 GALACTIC BULGE REGION LOW-MASS PHOTOIONIZATION DISTANCES EVOLUTION CATALOG STARS ABUNDANCES MOCASSIN CLASSIFICATION
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Abell 14 is a poorly studied object despite being considered a born-again planetary nebula. We performed a detailed study of its 3D morphology and ionization structure using the SHAPE and MOCASSIN codes. We found that Abell 14 is a highly evolved, bipolar nebula with a kinematical age of similar to 19 400 yr for a distance of 4 kpc. The high He abundance, and N/O ratio indicate a progenitor of 5 M-circle dot that has experienced the third dredge-up and hot bottom burning phases. The stellar parameters of the central source reveal a star at a highly evolved stage near to the white dwarf cooling track, being inconsistent with the born-again scenario. The nebula shows unexpectedly strong [N I] lambda 5200 and [O I] lambda 6300 emission lines indicating possible shock interactions. Abell 14 appears to be a member of a small group of highly evolved, extreme type-I planetary nebulae (PNe). The members of this group lie at the lower-left corner of the PNe regime on the [NII]/H alpha versus [S II]/H alpha diagnostic diagram, where shock-excited regions/objects are also placed. The low luminosity of their central stars, in conjunction with the large physical size of the nebulae, result in a very low photoionization rate, which can make any contribution of shock interaction easily perceptible, even for small velocities.
10.1093/mnras/stw038
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