Tides Between the TRAPPIST-1 Planets

Hamish C.F.C. Hay; Isamu Matsuyama

doi:10.3847/1538-4357/ab0c21

Tides Between the TRAPPIST-1 Planets

Hamish C.F.C. Hay, Isamu Matsuyama

Research output: Contribution to journal › Article › peer-review

13 Scopus citations

Abstract

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-viscosity (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^-3-10^-4 for most of the TRAPPIST-1 planets.

Original language	English (US)
Article number	22
Journal	Astrophysical Journal
Volume	875
Issue number	1
DOIs	https://doi.org/10.3847/1538-4357/ab0c21
State	Published - Apr 10 2019

Keywords

Gravitation
planets and satellites: Dynamical evolution and stability
planets and satellites: Individual (TRAPPIST-1g)
planets and satellites: Interiors
planets and satellites: Terrestrial planets

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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title = "Tides Between the TRAPPIST-1 Planets",

abstract = "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-viscosity (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 = 10-3-10-4 for most of the TRAPPIST-1 planets.",

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AU - Matsuyama, Isamu

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N2 - 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-viscosity (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 = 10-3-10-4 for most of the TRAPPIST-1 planets.

AB - 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-viscosity (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 = 10-3-10-4 for most of the TRAPPIST-1 planets.

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KW - planets and satellites: Dynamical evolution and stability

KW - planets and satellites: Individual (TRAPPIST-1g)

KW - planets and satellites: Interiors

KW - planets and satellites: Terrestrial planets

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Tides Between the TRAPPIST-1 Planets

Abstract

Keywords

ASJC Scopus subject areas

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