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Three dimensional Monte Carlo simulations of ionized nebulae

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Figure

Figure 1.1: Evolutionary path for an initially 3 M© star from the main sequence to the white dwarf
Figure 1.2; Evolution of a post-AGB model for a star with initial mass of 3 IVI© and remnant mass
Figure 1.3: Energy-level diagram for the lowest terms of [OIII] from ground 2p^ configuration
Figure 1.4; Transitions between O I I I  multiplets which occur following excitation of O I I I  2p3d
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