Photoionization model analysis of the planetary nebula Hu1-2

We have obtained high resolution optical spectra of the planetary nebula Hu 1-2 in the wavelength region of 3700 Å–10 050 Å, with the Hamilton Echelle Spectrograph (HES) at Lick Observatory. Diagnostic analysis indicates that the nebular gas can be represented by inhomogeneous shells of electron den...

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Bibliographic Details
Published in:Astronomy and astrophysics (Berlin) 2004-10, Vol.425 (1), p.143-149
Main Authors: Hyung, S., Pottasch, S. R., Feibelman, W. A.
Format: Article
Language:English
Subjects:
ISM: abundances
ISM: planetary nebulae: individual: Hu 1-2
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Summary:We have obtained high resolution optical spectra of the planetary nebula Hu 1-2 in the wavelength region of 3700 Å–10 050 Å, with the Hamilton Echelle Spectrograph (HES) at Lick Observatory. Diagnostic analysis indicates that the nebular gas can be represented by inhomogeneous shells of electron density $N_{\epsilon} \simeq$ 4000–10 000 cm-3, and a gas temperature of 12 000–18 000 K. Using the spherically symmetric photoionization model with appropriate abundances, we tried to accommodate the observed physical conditions and high electron temperatures. The chemical composition of the nebula was derived from calculations using a photoionization model which predicts the observed IUE, HES and ISO line intensities; and the composition was then compared to previous determinations. Model analysis confirms the semi-empirically determined abundance derivations carried out in earlier studies. He and N abundances are high, but those of C, O, Ne and S are very low.
ISSN:0004-6361
1432-0746
DOI:10.1051/0004-6361:20041005