The High-Excitation Planetary Nebula NGC 246: Optical and Near-Ultraviolet Observations and Two-dimensional Numerical Models

Details The High-Excitation Planetary Nebula NGC 246: Optical and Near-Ultraviolet Observations and Two-dimensional Numerical Models The High-Excitation Planetary Nebula NGC 246: Optical and Near-Ultraviolet Observations and Two-dimensional Numerical Models

Sep 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003apj...594..874s&link_type=abstract

The Astrophysical Journal, Volume 594, Issue 2, pp. 874-887.

Astronomy and Astrophysics

Astronomy

12

Stars: Circumstellar Matter, Hydrodynamics, Ism: Kinematics And Dynamics, Ism: Planetary Nebulae: Individual: Ngc Number: Ngc 246

Scientific paper

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-1, and include the time evolution of the wind parameters and UV radiation field from the progenitor star.

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