The subsurface habitability of small, icy exomoons

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Table 1

Planets (left) and moons (right) used as fiducial models.

	Saturn		Uranus
M_p (M_⊕)	95.159		14.536
R_p (10⁶ m)	58.232		25.362
α_p	0.342		0.3
x_p,exc	2.5		1.1
a_p (AU)	9.5826		19.2184
e_p	0.0565		0.0464
i_p (deg)	2.485		0.773

	Enceladus	Rhea	Titania	Oberon

Host planet	Saturn	Saturn	Uranus	Uranus
M_s (10²⁰ kg)	1.08	23.06	35.27	30.14
ρ_s (g cm⁻³)	1.61	1.24	1.72	1.63
α_s	0.81	0.70	0.17	0.14
ɛ_s	0.95	0.90	0.60	0.60
Φ_s	0.005	0.009	0.010	0.010
D_rego (m)	20	50	50	50
f_m,NH₃	0.00	0.10	0.15	0.15
a_s (10⁶ m)	237.95	527.11	435.91	583.52
e_s	0.0047	0.0013	0.0011	0.0014
i_s (deg)	26.74	27.08	98.11	97.83

Notes. We note that (1) emissivities are average estimates; (2) the values for x_p,exc are estimates; and 3) the inclinations listed here are equal to the inclinations of the moons relative to their host planets’ equators plus the hosts’ axial tilts.

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