Tides Between The TRAPPIST-1 Planets

The TRAPPIST-1 system is sufficiently closely packed that tides raised by one planet on another are significant. We investigate whether this source of tidal heating is comparable to eccentricity tides raised by the star.

Assuming a homogeneous body with a Maxwell rheology, we find that energy dissipation from stellar tides always dominates over that from planet-planet tides across a range of viscosities. TRAPPIST-1 g may experience the greatest proportion of planet-planet tidal heating, where it can account for between 2% and 20% of the total amount of tidal heating, for high (1021 Pa s) and low viscosity (1014 Pa s) regimes, respectively. If planet-planet tidal heating is to exceed that from stellar eccentricity tides, orbital eccentricities must be no more than e=10−3 to 10−4 for most of the TRAPPIST-1 planets.

Hamish Hay, Isamu Matsuyama
(Submitted on 11 Mar 2019)

Comments: 14 pages – 7 figures – accepted to ApJ
Subjects: Earth and Planetary Astrophysics (astro-ph.EP)
Cite as: arXiv:1903.04501 [astro-ph.EP] (or arXiv:1903.04501v1 [astro-ph.EP] for this version)
Submission history
From: Hamish Hay
[v1] Mon, 11 Mar 2019 18:00:02 UTC (1,108 KB)
https://arxiv.org/abs/1903.04501
Astrobiology