Convergent Migration Renders TRAPPIST-1 Long-lived

Tamayo, Daniel; Rein, Hanno; Petrovich, Cristóbal; Murray, Norman

doi:10.3847/2041-8213/aa70ea

Cited by 129 publications

(124 citation statements)

References 39 publications

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“…As an example, the comparison of the NAMD values of the solar system and TRAPPIST-1 suggests that the first was characterized by a relatively more violent or chaotic dynamical history than the second. This is consistent with the results of dynamical studies of the AMD-stability of the solar system (Laskar, 1997(Laskar, , 2000Laskar & Petit, 2017) and the formation and evolution of TRAPPIST-1 (Tamayo et al, 2017;Papaloizou et al, 2018).…”

Section: Discussionsupporting

confidence: 90%

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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Section: Discussionsupporting

confidence: 90%

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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“…To extract orbital parameters, we use the numerical integrations of Tamayo et al (2017), which simulated a range of initial conditions near the observed resonant configurations of TRAPPIST-1. These spanned configurations at or near the centers of the observed resonant chain where eccentricities and mean motions remain nearly constant (i.e., low spin forcing), to ones near their separatrices where the orbits undergo larger, chaotic oscillations (i.e., strong spin forcing).…”

Section: Setupmentioning

confidence: 99%

The chaotic nature of TRAPPIST-1 planetary spin states

Vinson

Tamayo

Hansen

2019

Monthly Notices of the Royal Astronomical Society

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The TRAPPIST-1 system has 7 known terrestrial planets arranged compactly in a mean motion resonant chain around an ultra-cool central star, some within the estimated habitable zone. Given their short orbital periods of just a few days, it is often presumed that the planets are tidally locked such that the spin rate is equal to that of the orbital mean motion. However, the compact, and resonant, nature of the system implies that there can be significant variations in the mean motion of these planets due to their mutual interactions. We show that such fluctuations can then have significant effects on the spin states of these planets. In this paper, we analyze, using detailed numerical simulations, the mean motion histories of the three planets that are thought to lie within or close to the habitable zone of the system: planets d, e, and f. We demonstrate that, depending on the strength of the mutual interactions within the system, these planets can be pushed into spin states which are effectively non-synchronous. We find that it can produce significant libration of the spin state, if not complete circulation in the frame co-rotating with the orbit. We also show that these spin states are likely to be unable to sustain long-term stability, with many of our simulations suggesting that the spin evolves, under the influence of tidal synchronization forces, into quasi-stable attractor states, which last on timescales of thousands of years.

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“…This is often interpreted as evidence for late inward migration from beyond the snow line, leading to scattering of interior planetesimals (Beauge & Nesvorný 2012;Spalding & Batygin 2017;Heller 2018;Dawson & Johnson 2018). E-mail: esandford@astro.columbia.edu At the other extreme, systems like Kepler-11 (Lissauer et al 2011a) and TRAPPIST-1 (Gillon et al 2017) pack half a dozen planets within the orbit of Mercury, which suggests that disk migration and resonant trapping may guide the evolution of such systems (Quillen 2006;Mustill & Wyatt 2011;Ormel et al 2017;Tamayo et al 2017;Papaloizou et al 2018).…”

Section: Introductionmentioning

confidence: 99%

The multiplicity distribution of Kepler’s exoplanets

Sandford

Kipping

Collins

2019

Monthly Notices of the Royal Astronomical Society

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The true multiplicity distribution of transiting planet systems is obscured by strong observational biases, leading low-multiplicity systems to be overrepresented in the observed sample. Using the Kepler FGK planet hosts, we employ approximate Bayesian computation to infer the multiplicity distribution by comparing simulated catalogs to the observed one. After comparing a total of ten different multiplicity distributions, half of which were two-population models, to the observed data, we find that a singlepopulation model following a Zipfian distribution is able to explain the Kepler data as well as any of the dichotomous models we test. Our work provides another example of a way to explain the observed Kepler multiplicities without invoking a dichotomous planet population. Using our preferred Zipfian model, we estimate that an additional 2393 +904 −717 planets likely reside in the 1537 FGK Kepler systems studied in this work, which would increase the planet count by a factor of 2.22 +0.46 −0.36 . Of these hidden worlds, 663 +158 −151 are expected to reside in ostensibly single-transiting-planet systems, meaning that an additional planet(s) is expected for approximately 1-in-2 such Kepler systems.

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Convergent Migration Renders TRAPPIST-1 Long-lived

Cited by 129 publications

References 39 publications

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

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

The chaotic nature of TRAPPIST-1 planetary spin states

The multiplicity distribution of Kepler’s exoplanets

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