The 3-D shaping of NGC 6741: a massive, fast-evolving Planetary Nebula at the recombination--reionization edge

Details The 3-D shaping of NGC 6741: a massive, fast-evolving Planetary Nebula at the recombination--reionization edge The 3-D shaping of NGC 6741: a massive, fast-evolving Planetary Nebula at the recombination--reionization edge

2005-02-04

arxiv.org/abs/astro-ph/0502101v1

Astronomy and Astrophysics

Astrophysics

27 pages, 18 figures, accepted for publication in A&A, movies of the reconstructed nebula are available at http://web.pd.astro

Scientific paper

10.1051/0004-6361:20042447

We infer the gas kinematics, diagnostics and ionic radial profiles, distance and central star parameters, nebular photo- ionization model, spatial structure and evolutionary phase of the PN NGC 6741 by means of long-slit high-resolution spectra at nine position angles. NGC 6741 (distance ~2.0 kpc, age ~1400 yr, ionized mass Mion ~0.06 Mo) is a dense (electron density up to 12,000 cm^(-3)), high-excitation, almost- prolate ellipsoid, surrounded by a sharp low-excitation skin (the ionization front), and embedded into a spherical (radius ~ 0.080 pc), almost-neutral, high-density (n(HI) ~7 x 10^3 atoms cm^(-3)) halo containing a large fraction of the nebular mass (Mhalo>0.20 Mo). The kinematics, physical conditions and ionic structure indicate that NGC 6741 is in a deep recombination phase, started about 200 years ago, and caused by the quick luminosity drop of the massive (M*=0.66-0.68 Mo), hot (logT* ~ 5.23) and faint (log L*/Lo ~ 2.75) post--AGB star, which has exhausted the hydrogen-shell nuclear burning and is moving along the white dwarf cooling sequence. The general expansion law of the ionized gas in NGC 6741, Vexp (km s^(-1)=13 x R", fails in the innermost, highest-excitation layers, which move slower than expected. The observed deceleration is ascribable to the luminosity drop of the central star, and appears in striking contrast to recent reports inferring that acceleration is a common property of the Planetary Nebulae innermost layers. Some general implications on the shaping mechanisms of Planetary Nebulae are discussed.

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