Hot-bubble structure of the WR100V05 simulation at t = 9107 yr, T_eff = 139 968 K, L_⋆ = 2841 L_⊙· Top: radial profile of electron temperature (dashed, right ordinate), electron density (dotted), and ion density (solid). The star is at r = 0, the wind’s reverse shock at R₁ = 2.5 × 10¹⁷ cm. The transition from the wind-shocked hydrogen-poor WR matter to the evaporated nebular PN matter is at r = 4.6 ×10¹⁷ cm (T ≃ 5.0 MK), the heat conduction front (bubble-nebula interface) at R₂ = 6.5 ×10¹⁷ cm, and the high-density region between 6.5 × 10¹⁷ and 8.3 × 10¹⁷ cm is the fully ionised planetary nebula proper with its double-shell structure and an electron temperature of about 1.2×10⁴ K. Middle: X-ray surface brightness distribution (6–11 Å) for the same model, assuming CIE, before (solid) and after (dashed) absorption by a hydrogen column density of N_H = 0.25 × 10²² cm⁻². The masses contained in the two bubble parts are 3.05 ×10⁻³ M_⊙ of WR matter, supplied by the stellar wind, and 4.24 ×10⁻³ M_⊙ of evaporated PN matter. Bottom: same as middle panel, but assuming NEI of nine key elements.