Asteroseismology of planetary nebula nuclei

Details Asteroseismology of planetary nebula nuclei Asteroseismology of planetary nebula nuclei

Oct 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aca....43..425b&link_type=abstract

Acta Astronomica, vol. 43, no. 4, p. 425-430

Mathematics

Logic

13

Astronomical Photometry, Planetary Nebulae, Pulsars, Seismology, Variable Stars, White Dwarf Stars, Charge Coupled Devices, Radial Distribution, Telescopes

Scientific paper

Nine planetary nebula nuclei (PNNS) are now known to be pulsating variables. All of them are O VI or PG 1159-type objects, with extreme hydrogen deficiency and high abundances of C and O. They are non-radial pulsators, with typical periods of 10 to 30 min, and their probable descendants are the shorter-period GW Vir (PG 1159-035) pulsating white dwarfs whose PNe have presumably dispersed. The pulsating PNNs are promising candidates for asteroseismological study, although there are already indications that such analyses will be complicated by highly variable power spectra. We present preliminary results from two campaigns of global photometry on the pulsating nuclei of NGC 1501 and Sanduleak 3, and from ground- and space-based searches for radial-mode pulsations in PNNs and white dwarfs.

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