EDP Sciences
Free access
Issue
A&A
Volume 400, Number 1, March II 2003
Page(s) 161 - 183
Section Formation, structure and evolution of stars
DOI http://dx.doi.org/10.1051/0004-6361:20021690


A&A 400, 161-183 (2003)
DOI: 10.1051/0004-6361:20021690

The 3-D ionization structure of NGC 6818: A Planetary Nebula threatened by recombination

S. Benetti1, E. Cappellaro2, R. Ragazzoni3, F. Sabbadin1 and M. Turatto1

1  INAF - Osservatorio Astronomico di Padova, vicolo dell'Osservatorio 5, 35122 Padova, Italy
2  INAF - Osservatorio Astronomico di Capodimonte, via Moiariello 11, 80131 Napoli, Italy
3  INAF - Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125, Italy

(Received 24 September 2002 / Accepted 11 November 2002 )

Abstract
Long-slit NTT+EMMI echellograms of NGC 6818 (the Little Gem) at nine equally spaced position angles, reduced according to the 3-D methodology introduced by Sabbadin et al. (2000a,b), allowed us to derive: the expansion law, the diagnostics and ionic radial profiles, the distance and the central star parameters, the nebular photo-ionization model, the 3-D reconstruction in He II, [O III] and [N II], the multicolor projection and a series of movies. The Little Gem results to be a young (3500 years), optically thin (quasi-thin in some directions) double shell ( $M_{\rm ion} \simeq 0.13~M_\odot$) at a distance of 1.7  kpc, seen almost equatorial on: a tenuous and patchy spherical envelope ( $r\simeq 0.090$ pc) encircles a dense and inhomogeneous tri-axial ellipsoid ( $a/2\simeq 0.077$ pc, $a/b\simeq 1.25$, $b/c \simeq 1.15$) characterized by a hole along the major axis and a pair of equatorial, thick moustaches. NGC 6818 is at the start of the recombination phase following the luminosity decline of the 0.625  $M_\odot$ central star, which has recently exhausted the hydrogen shell nuclear burning and is rapidly moving toward the white dwarf domain (log $T_*\simeq 5.22$ K; $\log L_*/L_\odot\simeq 3.1$). The nebula is destined to become thicker and thicker, with an increasing fraction of neutral, dusty gas in the outermost layers. Only over some hundreds of years the plasma rarefaction due to the expansion will prevail against the slower and slower stellar decline, leading to a gradual re-growing of the ionization front. The exciting star of NGC 6818 ( $m_{V}\simeq$17.06) is a visual binary: a faint, red companion ( $m_{V}\simeq$ 17.73) appears at 0.09 arcsec in PA $=190\degr$, corresponding to a separation $\ge$150 AU and to an orbital period $\ge$1500 years.


Key words: planetary nebulae: individual: NGC 6818 -- ISM: kinematics and dynamics

Offprint request: S. Benetti, benetti@pd.astro.it

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