THE COMPOSITIONAL DIVERSITY OF EXTRASOLAR TERRESTRIAL PLANETS. I. IN SITU SIMULATIONS

By J. Bond, D. O'Brien, Dante S. Lauretta. 2010

213 citations recorded by the source corpus.

Extrasolar planet host stars have been found to be enriched in key planet-building elements. These enrichments have the potential to drastically alter the composition of material available for terrestrial planet formation. Here, we report on the combination of dynamical models of late-stage terrestrial planet formation within known extrasolar planetary systems with chemical equilibrium models of the composition of solid material within the disk. This allows us to determine the bulk elemental composition of simulated extrasolar terrestrial planets. A wide variety of resulting planetary compositions are found, ranging from those that are essentially “Earth like,” containing metallic Fe and Mg silicates, to those that are dominated by graphite and SiC. This shows that a diverse range of terrestrial planets may exist within extrasolar planetary systems.

Subfields: Astronomy and Astrophysics, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/decc62ce943e9e0eb0b588883d3e7424350e470d

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Citations in the corpus

High-precision abundances of elements in solar twin stars - Trends with stellar age and elemental condensation temperature (2015, background): “This has led to speculations about the existence of exoplanets consisting of carbides and graphite insad of Earth-like silicates (Bond et al. 2010).”
C/O RATIO AS A DIMENSION FOR CHARACTERIZING EXOPLANETARY ATMOSPHERES (2012, background): “One of the most important quantities governing the chemistry in protoplanetary environments is the C/O ratio (Gilman 1969; Larimer 1974; Lodders & Fegley 1999; Lodders 2004; Kuchner & Seager 2005; Bond et al. 2010; Madhusudhan et al. 2011b; Oberg et al. 2011).”
MASS–RADIUS RELATION FOR ROCKY PLANETS BASED ON PREM (2015, background): “A Mg/Si ratio higher than 1 could produce more olivine (Mg2SiO4) or more MgO to affect the mineralogy of the upper mantle (Bond et al. 2010; Delgado Mena et al. 2010; Pagano et al. 2015).”
Tidal obliquity evolution of potentially habitable planets (2011, background): “Terrestrial bodies of such masses may have a variety of compositions (Bond et al. 2010), thus their response to tidal processes can vary.”
SWEET-Cat: A catalogue of parameters for Stars With ExoplanETs - I. New atmospheric parameters and masses for 48 stars with planets (2013, background): “…number, page 1 of 12 The chemical composition of a planet, both its interior and atmosphere, is also likely to be related to the chemical composition of the proto-stellar cloud, reflected on the composition of the stellar atmosphere (Guillot et al. 2006; Fortney et al. 2007; Bond et al. 2010).”
A dynamically-packed planetary system around GJ 667C with three super-Earths in its habitable zone (2013, background): “Hence precise calcultions of planetary composition are presently impossible, but see Bond et al. (2010); Carter-Bond et al. (2012) for some general trends.”
THE IMPRINT OF EXOPLANET FORMATION HISTORY ON OBSERVABLE PRESENT-DAY SPECTRA OF HOT JUPITERS (2016, background): “Other studies have proposed that carbon-rich planets could form around stars that have themselves intrinsically C/O>1 (e.g., Carter-Bond et al. 2010; Madhusudhan et al. 2012).”
Can we constrain the interior structure of rocky exoplanets from mass and radius measurements (2015, background): “Second, it has been demonstrated that during planet formation, planetary bulk and stellar ratios of Fe/Si and Mg/Si are very similar (e.g., Bond et al. 2010; Elser et al. 2012; Johnson et al. 2012; Thiabaud et al. 2014) since the refractory elements Fe, Si, and Mg condense at similar temperatures…”
A POSSIBLE CARBON-RICH INTERIOR IN SUPER-EARTH 55 Cancri e (2012, background): “Interiors of carbon-rich planets are expected to be composed of iron (Fe), carbon (C), SiC and/or silicates, depending on the thermal conditions where the planetesimals originated (Kuchner & Seager 2006; Bond et al. 2010; Carter-Bond et al. 2012; also see section 3).”
SPECTRAL PROPERTIES OF COOL STARS: EXTENDED ABUNDANCE ANALYSIS OF 1,617 PLANET-SEARCH STARS (2016, background): “Uniform analyses such as these minimize the relative errors in abundances, furthering our knowledge of planet formation (Santos et al. 2004; Fischer & Valenti 2005; Bond et al. 2010) and galactic structure and evolution (Bensby et al. 2014) and advancing progress in stellar astrophysics.”
Characterization of exoplanets from their formation - II. The planetary mass-radius relationship (2012, background): “In reality, due to the fact that stars do not have simply a scaled solar composition (e.g. Delgado Mena et al. 2010), there will be a spread both in the composition of refractory and volatile material in the planets (Bond et al. 2010).”
The Habitability of Planets Orbiting M-dwarf Stars (2016, background): “…for such an effect, based upon the hypothesis that planetesimal chemistry (and indeed, the presence or absence of planets) reflects the composition of oxygen-rich dust inherited from the molecular cloud (Barshay & Lewis, 1976; Bond et al., 2010; Moriarty et al., 2014; Gaidos et al., 2016a).”
The chemical diversity of exo-terrestrial planetary debris around white dwarfs (2012, background): “Extending the abundance studies of metal-polluted white dwarfs both in detail and number will provide further insight into the diversity of exo-terrestrial material, and guide the understanding of terrestrial exo-planet formation (Bond et al. 2010; Carter-Bond et al. 2012).”