Mathematics – Logic
Scientific paper
Dec 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufm.p31e..02j&link_type=abstract
American Geophysical Union, Fall Meeting 2010, abstract #P31E-02
Mathematics
Logic
[1027] Geochemistry / Composition Of The Planets, [6296] Planetary Sciences: Solar System Objects / Extra-Solar Planets
Scientific paper
The study of planetary systems around other stars is rapidly expanding to include spectral data on the composition of extrasolar planets. These can be interpreted in the context of what we know about the origin and evolution of our own solar system. Planetary characteristics are strongly affected by the composition of the solid material condensed from the protoplanetary stellar nebula in the planet forming regions, particularly the relative proportions of condensed volatile ices to refractory silicates and metals. This affects the relative amounts of enrichment of heavy elements and trapped volatiles of giant planets forming by core nucleated accretion and also the composition and evolution of rock-ice planetesimals which form satellites, Kuiper belt objects and asteroids, as well as solid, ‘terrestrial’ planets. Estimates of the rock-metal fraction of material incorporated by the ‘hot Jupiter’ HD 189733b have been used by Mousis et al. [1] to study the range of volatile abundances in the planet’s envelope. Since the parent star of HD 189733b has solar metallicity, solar abundance values from [2]were used, following the treatment of solar nebula condensates in [3]. However, while the compositions of main sequence stars are broadly similar to solar due to nucleosynthesis and the mixing of supernovae material, there are significant differences observed in the photospheric elemental abundances of the parent stars of extrasolar planets. We assume that this reflects equivalent differences in the composition of the protoplanetary nebulae from which these planets formed. Using data from two recent surveys of stars with extrasolar planets [4, 5] we have calculated the rock-metal fraction, fr-m, of ice-silicate condensates for 25 stars with a range of metallicity and composition. For solar composition fr-m varies from ~0.47 to ~0.76 depending on the redox state of C in the gas phase (CO-rich to CO-poor). The sample of extrasolar planet parent stars studied exhibits a significantly greater range, with fr-m ranging from less than 0.3 to 0.97; these values are correlated with the metalicity, [Fe] of the star and also strongly correlated with [C/O], which determines the amount of non-refractory O available to form water ice in CO-rich conditions. This raises the interesting possibility of both ‘dry’ extrasolar planetary systems with little or no water or other condensed volatiles, and ‘wet’ systems with water and volatile enhancements greater than seen in our solar system. [1] Mousis, O., et al. (2010) Astrophysical Journal Letters submitted. [2] Grevesse, N., et al. (2007) Space Sci. Rev. 130, 105-114. [3] Wong, M. H., et al., in Oxygen in the Solar System, G. J. MacPherson, Ed. (Mineralogical Society of America, Chantilly, VA, 2008), vol. Reviews in Mineralogy and Geochemistry Vol. 68, pp. 241-246. [4] Gonzales, G., et al. (2001) Astron. J. 121, 432-452. [5] TAKEDA, Y., et al. (2001) Publications of the Astronomical Society of Japan 53, 1211-1221.
Johnson Torrence V.
Lunine Jonathan I.
Mousis Oliver
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