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Asteroseismology of Planetary Nuclei

Published online by Cambridge University Press:  25 May 2016

Howard E. Bond ,
Steven D. Kawaler ,
Robin Ciardullo  and
Worldwide Collaborators
Howard E. Bond
Affiliation:
1Space Telescope Science Institute
Steven D. Kawaler
Affiliation:
2Iowa State University
Robin Ciardullo
Affiliation:
3Pennsylvania State University

Extract

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The first two pulsating planetary-nebula nuclei (PNNs), those of K 1-16 and Lo 4, were discovered by Grauer & Bond (1984) and Bond & Meakes (1990). They are nonradial multiperiodic g-mode pulsators, with typical periods near 25–31 min and low amplitudes (up to ∼ 0.05–0.1 mag). These PNNs have extremely high temperatures (Teff > 100,000 K), and are hydrogen-deficient with high abundances of C and O. Their spectra and pulsational properties are very similar to those of the pulsating GW Vir (PG 1159–035) white dwarfs.

Type
III. Central Stars
Information
Symposium - International Astronomical Union , Volume 180: Planetary Nebulae , 1997 , pp. 97 - 98
Copyright
Copyright © Kluwer 1997 

References

Bond, H. E., & Grauer, A. D. 1984, ApJ, 277, 211.Google Scholar
Bond, H. E., & Meakes, M. G. 1990, AJ, 100, 788.Google Scholar
Ciardullo, R. & Bond, H. E. 1996, AJ, 111, 2332.CrossRefGoogle Scholar
Kawaler, S. D., & Bradley, P. A. 1994, ApJ, 427, 415.CrossRefGoogle Scholar