Astrophys. J., 594, 874-887 (2003/September-2)
The high-excitation planetary nebula NGC 246: optical and near-ultraviolet observations and two-dimensional numerical models.
SZENTGYORGYI A., RAYMOND J., FRANCO J., VILLAVER E. and LOPEZ-MARTIN L.
Abstract (from CDS):
We have imaged the planetary nebula (PN) NGC 246 in the near-ultraviolet wavelengths [Ne V] 342.6 nm, the Bowen fluorescence line of O III at 344.4 nm, and a nearby line-free region centered on 338.6 nm, as well as Hα, [O III] 500.7 nm, and [S II] 673.0 and 671.5 nm. Imaging in the 344.4 nm line is necessary to deconvolve contamination of the [Ne V] images by O III 342.9 nm. The emission from the shell and inner parts of the nebula is detected in [Ne V]. The radial profiles of the [Ne V] brightness decrease with radius from the exciting star, indicating that the bulk of the emission from this ion is due to the hard UV stellar radiation field, with a (probably) marginal contribution from collisional ionization in a shock between the PN shell and the interstellar medium (ISM). In contrast, the radial profiles of the emission in Hα, [O III] 500.7 nm, and [S II] are flatter and peak at the location of the shell. The emission of [S II] probably traces the interaction of the PN with the ambient ISM. We also present two-dimensional numerical simulations for this PN-ISM interaction. The simulations consider the stellar motion with respect to the ambient ISM, with a velocity of 85 km/s, and include the time evolution of the wind parameters and UV radiation field from the progenitor star.
Stars: Circumstellar Matter - Hydrodynamics - ISM: Kinematics and Dynamics - ISM: Planetary Nebulae: Individual: NGC Number: NGC 246
Table 2: [SRF2003] NA (Nos 1A-1J, 2A-2E, 3A-3H, 4A-4G).
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