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Modeling hydrogen-deficient Planetary Nebulae
Published online by Cambridge University Press: 25 May 2016
Extract
Hydrogen-deficient planetary nebulae have central regions devoid of hydrogen. (See Harrington 1996 for a review of these nebulae.) They are characterized by exceptionally strong collisionally excited lines of [O III] and [Ne III], but relatively weak or undetected recombination lines of He or other elements. Such nebulae cannot be modeled successfully unless we include some source of heating in addition to photoionization by the central star.
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- IV. Envelopes
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- Copyright © Kluwer 1997