The spectrum of the central star of the planetary nebula in M22

Details The spectrum of the central star of the planetary nebula in M22 The spectrum of the central star of the planetary nebula in M22

Jul 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...411l.103h&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 411, no. 2, p. L103-L106.

Astronomy and Astrophysics

Astronomy

11

Asymptotic Giant Branch Stars, Globular Clusters, Planetary Nebulae, Stellar Spectra, Infrared Astronomy Satellite, Peculiar Stars, Stellar Composition

Scientific paper

New optical observations of the central star of the planetary nebula IRAS 18333-2357 in the globular cluster M22 show lines of H I, He II, C IV, N IV, and N V. The spectrum closely resembles the sdO star KS 292, which has surface abundances enhanced by products of hydrogen shell burning and helium burning, and an effective temperature of 75,000 K. The lines of C in IRAS 18333-2357 seem somewhat stronger than in KS 292, and the lines of N are considerably stronger. The presence of substantial hydrogen is surprising in view of the hydrogen-poor nature of the nebular ejecta. If IRAS 18333-2357 is as hot as its analog, its luminosity is about 14,000 lunar luminosity. This value is higher than that theoretically expected for single-star evolution of M22 cluster stars.

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