A new family of planets? Ocean-Planets

By A. Léger, F. Selsis, Christophe Sotin, T. Guillot, D. Despois, D. Mawet, M. Ollivier, A. Labèque, C. Valette, F. Brachet and 2 more. 2003

269 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/f169168f53cc0599317db1388c725f36955a169f

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In Astronomy and Astrophysics

Citations in the corpus

Toward a Deterministic Model of Planetary Formation. III. Mass Distribution of Short-Period Planets around Stars of Various Masses (2005, background): “Because these planets compose mostly of icy material and M stars’ luminosity is relatively weak, they may have water-vapor atmosphere and water ocean (Léger et al. 2004).”
Detailed Models of Super-Earths: How Well Can We Infer Bulk Properties? (2007, background): “These models were extended to super-Earths with large water content (Valencia et al. 2007)—the ocean planets proposed byKuchner (2003) and Leger et al. (2004).”
Water loss from terrestrial planets orbiting ultracool dwarfs: implications for the planets of TRAPPIST-1 (2016, background): “Both on the observational and theoretical side, it has been shown that planets could even have a large portion of their bulk made out of water (Ocean planets, hypothesized by Kuchner 2003; Léger et al. 2004; Ogihara & Ida 2009).”
The habitability of Proxima Centauri b. I. Irradiation, rotation and volatile inventory from formation to the present (2016, background): “Rather, they could be extremely water-rich (Kuchner 2003; Léger et al. 2004).”
Mass-Radius Relationships for Solid Exoplanets (2007, methodology): “As a second example, if we adopt a 6 M⊕ water planet similar to the Léger et al. (2004) water planet composed of 1 M⊕ Fe, 2 M⊕ silicates, and 3 M⊕ H2O, we find the total planet radius differs by less than 0.5% from that of our model with 45% water, 48.5% silicates, and 6.5% Fe.”
Transiting exoplanets from the CoRoT space mission VIII. CoRoT-7b: the first Super-Earth with measured radius (2009, unknown): “It can be either rocky or water-rich (Léger et al. 2004; Grasset etal.”
Exoplanet Atmospheres: Physical Processes (2010, background): “Other planets may have massive water vapor atmospheres (e.g., Leger et al. 2004; Rogers & Seager 2009).”
Radius and Structure Models of the First Super-Earth Planet (2006, background): “…and retain water as a major fraction (20% or more) of its total mass. Differentiation will quickly produce an Earth-like core and interior overlain by water ice (higher pressure ice phases such as VII and X) and a deep water ocean, similar to the ocean planets described by Léger et al. (2004).”
WATER LOSS FROM TERRESTRIAL PLANETS WITH CO2-RICH ATMOSPHERES (2013, unknown): “We use the term ‘ocean planet’ for any planet covered globally by liquid H2O, without any constraint on the total water volume (Léger et al. 2004; Fu et al. 2010).”
Ocean Planet or Thick Atmosphere: On the Mass-Radius Relationship for Solid Exoplanets with Massive Atmospheres (2007, background): “For short-period, low-mass planets, theoretical arguments of atmospheric escape may be the best way to identify a water world based on the mass and radius measurements alone (Léger et al. 2004; Selsis et al. 2007).”
Planetary Radii across Five Orders of Magnitude in Mass and Stellar Insolation: Application to Transits (2006, background): “Léger et al. (2004) have pointed out water-rich objects could reach many Earth masses (perhaps as failed giant planet cores) and migrate inward to smaller orbital distances.”
Making other earths: dynamical simulations of terrestrial planet formation and water delivery (2003, background): ““Water-rich” worlds may be so wet as to have a geologic evolution different from ours; “water worlds” are dominated by deep water mantles and remain speculative (Leger et al., 2003).”
ABIOTIC OZONE AND OXYGEN IN ATMOSPHERES SIMILAR TO PREBIOTIC EARTH (2014, background): “…values of Ffloor may be appropriate for planets with an oxidized bulk composition (compared to Earth), or for water-rich planets with high enough seafloor pressures that an ice VII layer forms at the ocean floor, potentially decreasing the flux of reduced mantle materials (Léger et al., 2004).”
3D climate modeling of close-in land planets: Circulation patterns, climate moist bistability and habitability (2013, background): “Not to be confused with an ocean planet for which, in addition, water must represent a significant fraction of the bulk mass (Léger et al. 2004). equilibrium balance and is heated until the surface can radiate at optical wavelength around a temperature of 1400 K (Kasting et al. 1984; Kasting 1988).”
Planet Formation around Stars of Various Masses: The Snow Line and the Frequency of Giant Planets (2007, background): “The outward movement of the snow line as stars more massive than the Sun reach the main-sequence, and as the disk becomes optically thin, allows the ocean planets suggested by Léger et al. (2004) to form in situ.”