Carbon Isotope Ratios in Planetary Nebulae: The Unexpected Enhancement of(13)C

Abstract

The(12)C/C-13 ratio has been measured toward a sample of planetary nebulae (PNe) using millimeter observations of CO, HCN, HNC, CN, and other species, conducted with the 12 m antenna and the Submillimeter Telescope of the Arizona Radio Observatory. The observed nebulae spanned the entire lifetime of PNe, from similar to 900 to 12,000 yr, and include well-known objects such as NGC 7293 (Helix), NGC 6720 (Ring), and NGC 2440, as well as relatively unexplored nebulae (M3-28, M2-48, and M3-55). In most cases, multiple molecules and transitions were used in the ratio determination, resulting in the most accurate values available to date, with 10%-40% uncertainties. The ratios found were unexpectedly low, lying in the range(12)C/C-13 similar to 1.0 0.7-13.2 4.9, with an average value of 3.7-drastically less than found in the envelopes of C-rich AGB stars, and, in some cases, lower than the minimum value achieved in equilibrium CNO burning. Such low values are expected for the two O-rich nebulae studied (M2-9 and M2-48), because of insufficient third dredge-up events. However, most of the PNe observed were clearly carbon-rich, as deduced from the large number of C-bearing molecules present in them. Because nucleosynthesis ceases in the PN stage, both the C/O and the(12)C/C-13 ratios must reflect abundances at the end of the AGB. These consistently low(12)C/C-13 ratios, combined with the bipolar/multipolar morphologies of all planetary nebulae observed, suggest an explosive process involving proton-capture occurred at the AGB-PN transition.