The nature of the TRAPPIST-1 exoplanets

Grimm, Simon L.; Demory, Brice-Olivier; Gillon, M.; Dorn, Caroline; Agol, Eric; Burdanov, Artem; Delrez, Laetitia; Sestovic, Marko; Triaud, A. H. M. J.; Turbet, Martin; Bolmont, Émeline; Caldas, Anthony; Wit, Julien de; Jehin, Emmanuël; Leconte, Jérémy; Raymond, Sean N.; Grootel, Valérie Van; Burgasser, Adam J.; Carey, Sean; Fabrycky, Daniel C.; Heng, Kevin; Hernández, David M.; Ingalls, James G.; Lederer, Susan M.; Selsis, Franck; Queloz, D.

doi:10.1051/0004-6361/201732233

Cited by 327 publications

(430 citation statements)

References 93 publications

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“…To the extent that neither material undergoes a transition such that the character of compression changes, uncertainties in the EoS of each account for ∼0.25% uncertainty in radius for a 4 M ⊕ planet. These uncertainties are less than the effect of variable CMF on radius for a given mass, as well as below the observational resolution for all but well‐resolved timed transit variation studies (e.g., Grimm et al, ). Similarly, the uncertainties in the EoS lead to just <2% uncertainty for central and CMB pressures (Figures b and d), and CMB temperature (Figure b).…”

Section: Resultsmentioning

confidence: 88%

The Pressure and Temperature Limits of Likely Rocky Exoplanets

Unterborn

Panero

2019

JGR Planets

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The interior composition of exoplanets is not observable, limiting our direct knowledge of their structure, composition, and dynamics. Recently described observational trends suggest that rocky exoplanets, that is, planets without significant volatile envelopes, are likely limited to <1.5 Earth radii. We show that given this likely upper limit in the radii of purely rocky super‐Earth exoplanets, the maximum expected core‐mantle boundary pressure and adiabatic temperature are relatively moderate, 630 GPa and 5000 K, while the maximum central core pressure varies between 1.5 and 2.5 TPa. We further find that for planets with radii less than 1.5 Earth radii, core‐mantle boundary pressure and adiabatic temperature are mostly a function of planet radius and insensitive to planet structure. The pressures and temperatures of rocky exoplanet interiors, then, are less than those explored in recent shock‐compression experiments, ab initio calculations, and planetary dynamical studies. We further show that the extrapolation of relevant equations of state does not introduce significant uncertainties in the structural models of these planets. Mass‐radius models are more sensitive to bulk composition than any uncertainty in the equation of state, even when extrapolated to terapascal pressures.

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Section: Resultsmentioning

confidence: 88%

The Pressure and Temperature Limits of Likely Rocky Exoplanets

Unterborn

Panero

2019

JGR Planets

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“…Looking beyond our solar system, the representation reported here encompassing all ice polymorphs and liquid water up to 2,300 MPa is also relevant for the study of exoplanets interiors and their potential habitability. This is especially true for water worlds like the ones proposed in the TRAPPIST-1 system (Grimm et al, 2018;Unterborn et al, 2018). The self-consistent thermodynamic properties for water and its ices provided by SeaFreeze can be used to accurately study the interior structure and evolution of watery exoplanets (Noack et al, 2016), computing of radius-mass curves (Sotin & Grasset, 2007;Unterborn et al, 2018), as well as studying their habitability and the effects of possible snow-ball regime on ocean words (Kite & Ford, 2018;Ramirez & Levi, 2018).…”

Section: Discussion and Perspectivesmentioning

confidence: 99%

Holistic Approach for Studying Planetary Hydrospheres: Gibbs Representation of Ices Thermodynamics, Elasticity, and the Water Phase Diagram to 2,300 MPa

et al. 2020

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Gibbs energy representations for ices II, III, V, and VI are reported. These were constructed using new measurements of volumes at high pressure over a range of low temperatures combined with calculated vibrational energies grounded in statistical physics. The collection of representations are released within the open source SeaFreeze program, together with the Gibbs representation already known for ice Ih and water. This program allows accurate determination of thermodynamics properties (phase boundaries, density, specific heat, bulk modulus, thermal expansivity, chemical potentials) and seismic wave velocities over the entire range of conditions encountered in hydrospheres in our solar system (130-500 K to 2,300 MPa). These comprehensive representations allow exploration of the rich spectrum of thermodynamic behavior in the H 2 O system. Although these results are broadly applicable in science and engineering, their use is particularly relevant to habitability analysis, interior modeling, and future geophysical sounding of water-rich planetary bodies of our solar system and beyond. Key Points:• New X-Ray diffraction measurements covering the entire range of ice II, III, V and VI using state of the art high pressure techniques • The first Gibbs energy equations of states for ice II, III, V and VI (and first equations of state for ice II, III and V) • New open-source code SeaFreeze allows to explore water and ices thermodynamic at all conditions found in solar system planetary hydrospheres Supporting Information:• Supporting Information S1

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“…The data collected for the various exoplanetary systems are updated to November 19, 2019, with the exception of TRAPPIST-1 for which we adopted the values of the planetary masses, semimajor axes, and eccentricities estimated by Grimm et al (2018), as they are more complete and precise than those currently present in the NASA Exoplanet Archive.…”

Section: Methodsmentioning

confidence: 99%

Normalized angular momentum deficit: a tool for comparing the violence of the dynamical histories of planetary systems

Turrini

Zinzi

Belinchón

2020

A&A

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Context. Population studies of the orbital characteristics of exoplanets in multi-planet systems have highlighted the existence of an anticorrelation between the average orbital eccentricity of planets and the number of planets of their host system, that is, its multiplicity. This effect was proposed to reflect the varying levels of violence in the dynamical evolution of planetary systems. Aims. Previous work suggested that the relative violence of the dynamical evolution of planetary systems with similar orbital architectures can be compared through the computation of their angular momentum deficit (AMD). We investigated the possibility of using a more general metric to perform analogous comparisons between planetary systems with different orbital architectures. Methods. We considered a modified version of the AMD, the normalized angular momentum deficit (NAMD), and used it to study a sample of 99 multi-planet systems containing both the currently best-characterized extrasolar systems and the solar system, that is, planetary systems with both compact and wide orbital architectures. Results. We verified that the NAMD allows us to compare the violence of the dynamical histories of multi-planet systems with different orbital architectures. We identified an anticorrelation between the NAMD and the multiplicity of the planetary systems, of which the previously observed eccentricity-multiplicity anticorrelation is a reflection. Conclusions. Our results seem to indicate that phases of dynamical instabilities and chaotic evolution are not uncommon among planetary systems. They also suggest that the efficiency of the planetary formation process in producing high-multiplicity systems is likely to be higher than that suggested by their currently known population.

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The nature of the TRAPPIST-1 exoplanets

Cited by 327 publications

References 93 publications

The Pressure and Temperature Limits of Likely Rocky Exoplanets

The Pressure and Temperature Limits of Likely Rocky Exoplanets

Holistic Approach for Studying Planetary Hydrospheres: Gibbs Representation of Ices Thermodynamics, Elasticity, and the Water Phase Diagram to 2,300 MPa

Normalized angular momentum deficit: a tool for comparing the violence of the dynamical histories of planetary systems

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