How internal structure shapes the metallicity of giant exoplanets

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Table 1

Power-law fit parameters (y = β M^α) derived from Bayesian regressions for the four interior-structure models.

Model	(a) M_Z–M		(b) Z–M
	α	β	α	β
CE	0.67 ± 0.11	35.9 ± 4.5	−0.33 ± 0.12	0.113 ± 0.014
DCA	0.70 ± 0.10	43.1 ± 4.4	−0.30 ± 0.10	0.136 ± 0.015
DCA3	0.72 ± 0.07	56.0 ± 4.2	−0.28 ± 0.07	0.176 ± 0.014
FM	0.65 ± 0.07	59.6 ± 4.4	−0.35 ± 0.07	0.187 ± 0.014

Notes. Parameters α and β correspond to the best-fit power-law relations M_Z = β M^α and Z = β M^α. Quoted values are posterior medians from Bayesian fits; typical 1σ uncertainties are σ_α ≃ 0.07 and σ_β ≃ 4.5 for M_Z–M, and σ_α ≃ 0.07, σ_β ≃ 0.014 for Z–M.

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