Modeling climate diversity, tidal dynamics and the fate of volatiles on TRAPPIST-1 planets

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Table 1

Adopted planetary characteristics of TRAPPIST-1 planets for climate simulations.

Parameter	Tb	Tc	Td	Te	Tf	Tg	Th	Unit
R_p	1.09^a	1.06^a	0.77^a	0.92^a	1.05^a	1.13^a	0.75^b	R_⊕
M_p	0.85^a	1.38^a	0.41^a	0.62^a	0.68^a	1.34^a	0.38 (arb.)	M_⊕
g_p	7.07	12.14	6.75	7.22	6.11	10.34	6.6 (arb.)	m s⁻²
Semi-major axis	0.011^a	0.015^a	0.021^a	0.028^a	0.037^a	0.045^a	0.060^b	au
S_p	4.25^a	2.27^a	1.143^a	0.662^a	0.382^a	0.258^a	0.165^b	S_⊕
S_p	5806	3101	1561	904	522	352	225	W m⁻²
Spin-orbit resonance				1:1
Period	1.51^a	2.42^a	4.05^a	6.10^a	9.21^a	12.35^a	18.76^b	Earth days
Ω_p	4.82	3.00	1.80	1.19	0.790	0.589	0.388	10⁻⁵ rad s⁻¹
Obliquity				0				°
Eccentricity				0

Notes. Most of the values derive from Gillon et al. (2017)^(a) and Luger et al. (2017)^(b). Note that mass estimates are all compatible (at less than 1σ) with the TTV analysis of Wang et al. (2017) that included both Spitzer (Gillon et al. 2017) and K2 (Luger et al. 2017) transits.

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