The minimum-mass extrasolar nebula: in situ formation of close-in super-Earths
Eugene Chiang,Gregory Laughlin +1 more
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TLDR
In this paper, the authors constructed the minimum-mass extrasolar nebula (MMEN), the circumstellar disk of solar-composition solids and gas from which such planets formed, if they formed near their current locations and did not migrate.Abstract:
Close-in super-Earths, with radii R = 2-5 R_Earth and orbital periods P < 100 days, orbit more than half, and perhaps nearly all Sun-like stars in the universe. We use this omnipresent population to construct the minimum-mass extrasolar nebula (MMEN), the circumstellar disk of solar-composition solids and gas from which such planets formed, if they formed near their current locations and did not migrate. In a series of back-of-the-envelope calculations, we demonstrate how in-situ formation in the MMEN is fast, efficient, and can reproduce many of the observed properties of close-in super-Earths, including their gas-to-rock fractions. Testable predictions are discussed.read more
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Seven temperate terrestrial planets around the nearby ultracool dwarf star TRAPPIST-1
Michaël Gillon,Amaury H. M. J. Triaud,Brice-Olivier Demory,Emmanuel Jehin,Eric Agol,Katherine M. Deck,Susan M. Lederer,Julien de Wit,Artem Burdanov,James G. Ingalls,Emeline Bolmont,Jérémy Leconte,Sean N. Raymond,Franck Selsis,Martin Turbet,Khalid Barkaoui,Adam J. Burgasser,Matthew R. Burleigh,Sean Carey,Aleksander Chaushev,Chris M. Copperwheat,Laetitia Delrez,Catarina S. Fernandes,Daniel Luke Holdsworth,Enrico J. Kotze,Valérie Van Grootel,Y. Almleaky,Zouhair Benkhaldoun,Pierre Magain,Didier Queloz +29 more
TL;DR: The observations reveal that at least seven planets with sizes and masses similar to those of Earth revolve around TRAPPIST-1, and the six inner planets form a near-resonant chain, such that their orbital periods are near-ratios of small integers.
Journal ArticleDOI
The California-Kepler Survey. III. A Gap in the Radius Distribution of Small Planets*
Benjamin J. Fulton,Erik A. Petigura,Andrew W. Howard,Howard Isaacson,Geoffrey W. Marcy,Phillip A. Cargile,Leslie Hebb,Lauren M. Weiss,John Asher Johnson,Timothy D. Morton,Evan Sinukoff,Ian J. M. Crossfield,Lea A. Hirsch +12 more
TL;DR: The size of a planet is an observable property directly connected to the physics of its formation and evolution as discussed by the authors, and the size of close-in (P < 100 days) small planets can be divided into two size regimes: R_p < 1.5 R⊕ or smaller with varying amounts of low-density gas that determine their total sizes.
Journal ArticleDOI
The Occurrence and Architecture of Exoplanetary Systems
TL;DR: A review of the current knowledge of the occurrence of planets around other stars, their orbital distances and eccentricities, the orbital spacings and mutual inclinations in multi-planet systems, the orientation of the host star's rotation axis, and the properties of planets in binary-star systems can be found in this paper.
Journal ArticleDOI
Most 1.6 earth-radius planets are not rocky
TL;DR: In this article, the authors apply a hierarchical Bayesian statistical approach to the sample of Kepler transiting sub-Neptune planets with Keck RV follow-up, constrain the fraction of close-in planets (with orbital periods less than ~50 days) that are sufficiently dense to be rocky, as a function of planet radius.
Journal ArticleDOI
Understanding the mass-radius relation for sub-neptunes: radius as a proxy for composition
TL;DR: In this paper, the authors provide model radii for low-mass rocky super-Earths with hydrogen-helium envelopes, with envelope fractions 0.01-20 M ⊕, with levels of irradiation 0.1-1000 times Earth's, and ages from 100 Myr to 10 Gyr.
References
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Solar System Abundances and Condensation Temperatures of the Elements
TL;DR: In this article, solar photospheric and meteoritic CI chondrite abundance determinations for all elements are summarized and the best currently available photosphere abundances are selected, including the meteoritic and solar abundances of a few elements (e.g., noble gases, beryllium, boron, phosphorous, sulfur).
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Solar system dynamics
TL;DR: In this paper, the two-body problem and the restricted three body problem are considered. And the disturbing function is extended to include the spin-orbit coupling and the resonance perturbations.
Solar system dynamics
TL;DR: In this paper, the two-body problem and the restricted three body problem are considered. But the disturbing function is defined as a special case of the two body problem and is not considered in this paper.
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