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2005MNRAS.360..499M - Mon. Not. R. Astron. Soc., 360, 499-508 (2005/June-3)
Modelling of aspherical nebulae - I. A quick pseudo-3D photoionization code.
MORISSET C., STASINSKA G. and PENA M.
Abstract (from CDS):
We present and comment upon line intensity maps corresponding to different viewing angles. We also use the computed line intensities to derive physical properties of the model in the same way as an observer would do for a real object. For example, we derive the `apparent' value of N/O for the entire nebula and along spectral slits of different orientations. For this, we take the electron temperature and density derived from the [Nii]5755Å/[Nii]6583Åand [Oii]3726Å/[Oii]3729Åratios, respectively, and we adopt the common recipe: N/O = N+/O+. Interestingly, we find that, in the case of our high-excitation nebula, the derived N/O is within 10-20 per cent of the real value, even when the slit crosses the high-density knots. On the other hand, for the blister Hii region and its spherical impostor, we find that the apparent N/O is much smaller than the true one (about 0.68 and 0.5 of it, respectively).
These two examples warn against preconceived ideas when interpreting spectroscopic and imaging data of Hii regions and planetary nebulae. The tools nebu{lowbar}3d and visneb{lowbar}3d, which will be made publicly available in the future, should facilitate the performance of numerical experiments, to yield a better understanding of the physics of aspherical ionized nebulae.
Abstract Copyright: 2005 RAS
Journal keyword(s): methods: numerical - ISM: abundances - Hii regions - planetary nebulae: general
Simbad objects: 6
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