Other
Scientific paper
Mar 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...290..568k&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 290, March 15, 1985, p. 568-577. Research supported by the University of Ca
Other
26
Astrometry, Distance, Planetary Nebulae, Lyman Spectra, Radiant Flux Density, Radio Emission, Stellar Evolution, Stellar Models
Scientific paper
The evolution of the ionization structure of planetary nebulae is calculated from the central-star evolutionary models of Schoenberner (1983). The predictions of models in the 0.57-064 solar mass range are found to be consistent with observed nebular parameters of planetary nebulae with known distances. The rapid evolution of the central stars in the Schoenberner models implies that the nebular and central star evolutions are strongly coupled with each other, and interpretations of the nebular properties have to take into account the state of the central star. A semiempirical mass-radius relationship of the form M varies as R to the (beta) power, where beta = 2.25-2.50. This relationship suggests that the dependence of the radio flux density on angular size as the result of the expansion of an ionization front has approximately the same form as the flux-angular size dependence for planetary nebulae at different distances. Consequenty, distances of ionization-bounded planetary nebulae cannot be reliably determined from the measurement of radio flux (or H-beta) and angular size alone.
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