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Bi-abundance Photoionization Models for Planetary Nebulae

  • D. Péquignot (a1), X.-W. Liu (a2), M. J. Barlow (a2), P. J. Storey (a2) and C. Morisset (a3)...

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A new class of planetary nebulae, in which abundances derived from optical recombination lines (ORL) seem to be much larger than those derived from collisionally excited lines (CEL) by up to one or two orders of magnitude is now well identified (Liu, these proceedings and references therein).

Photoionization models including two components, one highly enriched in C, N, O, Ne and deficient in H and the other one of more usual composition, can account for most of the numerous spectroscopic data available from UV to far-IR in two of the best observed, most extreme examples, namely NGC 6153 and M142 (Péquignot et aI., 2002, and in preparation). The few discrepancies left can generally be understood in terms of inaccuracy of the observations (calibration of infrared line fluxes relative to the optical) and some atomic data, particularly in the unusual conditions prevailing in the H-deficient component.

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References

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Garnett, D. R., Dinerstein, H. L., 2001, ApJ, 558, 145
Liu, X.-W., Storey, P. J., Barlow, M. J., et al. 2000, MNRAS, 312, 585
Peimbert, M., 1967, ApJ, 150, 825
Quignot, et al., 2002, Rev. Mex. Astron. Astrofis., Ser de Conferencias, 12, 142

Bi-abundance Photoionization Models for Planetary Nebulae

  • D. Péquignot (a1), X.-W. Liu (a2), M. J. Barlow (a2), P. J. Storey (a2) and C. Morisset (a3)...

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