Mass–radius curve for extrasolar Earth-like planets and ocean planets

By Christophe Sotin, O. Grasset, A. Mocquet. 2007

345 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/4eb45b21e1be72109282bf481cbb1d4e11bd5e06

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Citations in the corpus

THE COMPOSITIONAL DIVERSITY OF EXTRASOLAR TERRESTRIAL PLANETS. I. IN SITU SIMULATIONS (2010, methodology): “Approximate planetary radii were obtained from Sotin et al. (2007) based on planetary mass.”
GLIESE 581D IS THE FIRST DISCOVERED TERRESTRIAL-MASS EXOPLANET IN THE HABITABLE ZONE (2011, methodology): “2M Earth, given that the statistically most probable value for the inclination angle is 60. Radius and gravity for rocky and ocean / ice cases (Table 1) were then determined from theoretical models (Sotin et al. 2007). In the latter case, the assumed bulk composition of the planet was 50% H 2O. Mode”
Can we constrain the interior structure of rocky exoplanets from mass and radius measurements (2015, background): “Sotin et al. (2007) showed that rocky planets can be described with great accuracy by only using the four elements Si, Mg, Fe, O.”
Transiting exoplanets from the CoRoT space mission VIII. CoRoT-7b: the first Super-Earth with measured radius (2009, neutral): “The estimated radius (1.68± 0.09 REarth) and mass limit (< 21 MEarth) of the planet can be located in the (R, M) plane and compared with the R(M) relations derived from the modellings of the internal structures of different planets (Sotin et al. 2007; Elkins-Tanton & Seager 2008; Valencia etl.”
Tidal locking of habitable exoplanets (2017, methodology): “For the planet, I used the mass–radius relationship of Sotin et al. (2007) for planets with Earth-like composition:”
FORMATION AND STRUCTURE OF LOW-DENSITY EXO-NEPTUNES (2011, background): “Fol- 10 lowing an approach similar to Sotin et al. (2007), less abundant elements are represented by their most similar neighbors in the periodic table: metallic Ni is added to metallic Fe, Ca is added to Mg, and Al is divided equally (by number) between Si and Mg to preserve charge conservation.”
Tidal obliquity evolution of potentially habitable planets (2011, neutral): “The relationship betweenMp and the planetary radiusRp is taken asRp = (Mp/MEarth)0.27 × REarth (Sotin et al. 2007).”
A POSSIBLE CARBON-RICH INTERIOR IN SUPER-EARTH 55 Cancri e (2012, methodology): “Our model solves the three canonical equations of internal structure for solid planets, namely, (a) mass conservation, (b) hydrostatic equilibrium, and (c) the equation of state (e.g. Fortney et al. 2007; Seager et al. 2007; Sotin et al. 2007; Valencia et al. 2007; Rogers & Seager 2010).”
DETECTION OF AN ATMOSPHERE AROUND THE SUPER-EARTH 55 CANCRI E (2015, background): “Even basic information about their density seems to suggest that there is a variety of cases (e.g. Sotin et al. 2007; Grasset et al. 2009; Valencia et al. 2007, 2013; Zeng & Sasselov 2014).”
PLANET OCCURRENCE WITHIN 0.25 AU OF SOLAR-TYPE STARS FROM KEPLER (2011, background): “Placing these wellmeasured planets on theoretical mass–radius relationships (e.g., Valencia et al. 2006; Seager et al. 2007; Sotin et al. 2007; Baraffe et al. 2008; Grasset et al. 2009) provides insight into the range of compositions encompassed by the detected planets.”
Ocean Planet or Thick Atmosphere: On the Mass-Radius Relationship for Solid Exoplanets with Massive Atmospheres (2007, background): “Most authors have assumed that solid planets in the 5 to 10 M⊕ range have an insignificant amount of hydrogen (Valencia et al. 2006a,b; Fortney et al. 2007; Seager et al. 2007; Selsis et al. 2007; Sotin et al. 2007).”
Mantle dynamics in super-Earths: Post-perovskite rheology and self-regulation of viscosity (2012, background): “Initial studies focused on determining the radial structure of such planets (Seager et al., 54 2007; Sotin et al., 2007; Valencia et al., 2006; Valencia et al., 2007b; Valencia et al., 2007c).”