Bibcode
Corradi, R. L. M.; Rodríguez-Gil, P.; Jones, D.; García-Rojas, J.; Mampaso, A.; García-Alvarez, D.; Pursimo, T.; Eenmäe, T.; Liimets, T.; Miszalski, B.
Bibliographical reference
Monthly Notices of the Royal Astronomical Society, Volume 441, Issue 4, p.2799-2808
Advertised on:
7
2014
Citations
31
Refereed citations
26
Description
While analysing the images of the IPHAS (INT/WFC Photometric Hα
Survey of the northern Galactic plane) survey, we noticed that the
central star of the candidate planetary nebula IPHASXJ211420.0+434136
(also named Ou5) was clearly variable. This is generally considered as
an indication of binarity. To confirm it, we performed a photometric
monitoring of the central star, and obtained images and spectra of the
nebula. The nebular spectrum confirms that IPHASXJ211420.0+434136 is a
planetary nebula of moderately high excitation. It has a remarkable
morphology with two nested pairs of bipolar lobes and other unusual
features. The light curve of the central star reveals that it is an
eclipsing binary system with an orbital period of 8.74 h. It also
displays a strong irradiation effect with an amplitude of 1.5 mag. The
presence of multiple bipolar outflows adds constraints to the formation
of these nebulae, suggesting the occurrence of discrete ejection events
during, or immediately before, the common-envelope phase.
IPHASXJ211420.0+434136 also adds evidence to the hypothesis that a
significant fraction of planetary nebulae with close binary central
stars have a peculiar nebular chemistry and a relatively low nebular
mass. This may point to low-mass, low-metallicity progenitors, with
additional effects related to the binary evolution. We also suggest that
these objects may be relevant to understand the abundance discrepancy
problem in planetary nebulae.
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