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تسجيل مستخدم جديدAnalysis of chemical abundances in planetary nebulae with [WC] central stars. I. Line intensities and physical conditions
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(Abridged) Planetary nebulae (PNe) around Wolf-Rayet [WR] central stars ([WR]PNe) constitute a particular photoionized nebula class that represents about 10% of the PNe with classified central stars. We analyse deep high-resolution spectrophotometric data of 12 [WR]PNe. This sample represents the most extensive analysed so far, at such high spectral resolution. We aim to select the optimal physical conditions in the PNe to be used in ionic abundance calculations that will be presented in a forthcoming paper. We acquired spectra at LCO with the 6.5-m telescope and the MIKE spectrograph, covering a wavelength range from 3350 to 9400 A. The spectra were exposed deep enough to detect, with signal-to-noise ratio higher than three, the weak ORLs of OII, CII, and other species. We detect and identify about 2980 emission lines, which, to date, is the most complete set of spectrophotometric data published for this type of objects. From our deep data, numerous diagnostic line ratios for Te and Ne are determined from CELs, ORLs, and continuum measurements. Densities are closely described by the average of all determined values for objects with ne<10^4 cm-3, and by ne([Cl III]) for the densest objects. For Te, we adopt a three-zone ionization scheme, where the low ionization zone is characterized by Te([NII]), the medium ionization zone by Te([OIII]) and the highest ionization one by Te([ArIV]) when available. We compute Te from the HI Paschen discontinuity and from HeI lines. We do not find evidences of the presence of low-temperature, high-density clumps in our [WR]PNe from the analysis of faint O II and N II plasma diagnostics. The behaviour of Te([OIII])/Te([NII]) being very low for high ionization degrees can be reproduced by a set of combined matter-bounded and radiation-bounded models, however, for the lowest temperature ratios, too high metallicity seem required.
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(Abridged) We present the abundance analysis of 12 PNe ionized by [WC]-type stars and wels obtained from high-resolution spectrophotometric data. Our main aims are to determine the chemical composition of the PNe and to study the behaviour of the abu
ndance discrepancy problem (ADF) in this type of planetary nebulae. The detection of a large number of optical recombination lines (ORLs) and collisionally excited lines (CELs) from different ions were presented previously. Most of the ORLs were reported for the first time in these PNe. Ionic abundances were derived from the available CELs and ORLs, using previously determined physical conditions. Based on these two sets of ionic abundances, we derived the total chemical abundances in the nebulae using suitable ICFs (when available). In spite of the [WC] nature of the central stars, moderate ADF(O^++), in the range from 1.2 to 4, were found for all the objects. We found that when the quality of the spectra is high enough the ORLs O^++/H^+ abundance ratios obtained from different multiplets excited mainly by recombination are very similar. Possible dependence of ADFs with some nebular characteristics were analysed, finding no correlation. Abundances derived from CELs were corrected by determining the t^2 parameter. O abundances for PNe, derived from ORLs, are in general larger than the solar abundance. We derived the C/O ratio from ORLs and N/O and alpha-element/O ratios from CELs and found that these PNe are, in average, N-and C-richer than the average of large PN samples. About half of our sample is C-rich (C/O>1). The alpha-elements grow in lockstep with O abundance. Comparing the N/O and C /O ratios with those derived from stellar evolution models, we estimate that about half of our PNe have progenitors with initial masses > 4 M_sun. No correlation was found between the stellar [WC]-type and the nebular abundances.
We present preliminary results obtained from the analysis of very deep echelle spectra of a dozen planetary nebulae with [WC] or weak emission lines (wels) central stars. The computed abundance discrepancy factors (ADFs) are moderate, with values low
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The kinematic structure of a sample of planetary nebulae, consisting of 23 [WR] central stars, 21 weak emission line stars (wels) and 57 non-emission line central stars, is studied. The [WR] stars are shown to be surrounded by turbulent nebulae, a ch
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