Interior structures and tidal heating in the TRAPPIST-1 planets

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Table 2

Inner structure of the planets for maximum, minimum and mean bulk densities.

Planet	ϕ_Fe	ϕ_r	ϕ_hpp	ϕ_I	R_fe [km]	R_r [km]	R_hpp [km]	R_I [km]
	0.006	0.994	–	–	1204	6696	–	–
b	0.121	0.221	0.644	0.014	3418	4839	6887	6919
	–	0.201	0.777	0.021	–	4185	7090	7142

	0.960	0.040	–	–	6418	6505	–	–
c	0.377	0.623	–	–	4862	6728	–	–
	–	0.799	0.191	0.011	–	6449	6925	6951

	0.212	0.788	–	–	2820	4727	–	–
d	–	0.721	0.256	0.023	–	4410	4880	4918
	–	0.173	0.783	0.044	–	2846	5034	5110

	0.215	0.785	–	–	3353	5600	–	–
e	–	0.115	0.848	0.038	–	2841	5774	5849
	–	0.007	0.947	0.046	–	1158	6003	6097

	–	0.352	0.627	0.021	–	4529	6371	6416
f	–	0.122	0.850	0.029	–	3299	6593	6658
	–	0.005	0.959	0.036	–	1209	6816	6900

	–	0.354	0.628	0.018	–	4893	6877	6919
g	–	0.240	0.740	0.020	–	4463	7132	7180
	–	0.145	0.833	0.022	–	3908	7386	7441

	–	0.930	0.031	0.039	–	4154	4200	4256
h	–	0.012	0.907	0.081	–	1031	4429	4555

Notes. The table lists: volume fraction (ϕ) and radius (R) of the top ofiron, rock, high-pressure ice polymorphs, and ice I/water layers in each of the seven TRAPPIST-1 exoplanets. Maximum mass and minimum radius (as indicated in Table 1) were assumed for the calculations indicated by , and similarly, minimum mass and maximum radius were assumed for the cases. ^(*) For these models, ρ_r = 3300 kg m⁻³ (see Sect. 2.2).

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