Core masses and abundances of low-excitation planetary nebulae in the Magellanic Clouds

Details Core masses and abundances of low-excitation planetary nebulae in the Magellanic Clouds Core masses and abundances of low-excitation planetary nebulae in the Magellanic Clouds

Nov 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...382..134k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 382, Nov. 20, 1991, p. 134-142.

Astronomy and Astrophysics

Astrophysics

33

Abundance, Magellanic Clouds, Planetary Nebulae, Stellar Cores, Stellar Mass, Carbon, Helium, Nitrogen, Oxygen, Stellar Composition, Stellar Evolution

Scientific paper

Core masses and chemical compositions for luminous low-excitation planetary nebulae in the Magellanic Clouds are derived. They are all on horizontal evolutionary tracks with core masses that concentrate between 0.55 and 0.6 solar mass, and have low He/H and N/O ratios as expected from the relation found by Kaler and Jacoby (1990, 1990). It is suggested that C/O anticorrelates with N/O; below 0.63 solar mass, O/H correlates positively with core mass. In combination with previous studies, accurate core masses are determined for 80 planetaries in the Magellanic Clouds. Of these, 33 are members of a bright sample, defined as the set of 50 that fall in the top 1.5 mag of the forbidden O III luminosity function. Excellent agreement is found between the core mass distribution of this group and the prediction of Jacoby (1989) that O-III-forbidden-bright planetaries have a very narrow Gaussian high-mass cutoff. The distribution of core masses on the log L-log T plane is qualitatively consistent with theoretical evolutionary rates.

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