2016
DOI: 10.3847/0004-637x/831/1/64
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The Mass–metallicity Relation for Giant Planets

Abstract: Exoplanet discoveries of recent years have provided a great deal of new data for studying the bulk compositions of giant planets. Here we identify 47 transiting giant planets (20M ⊕ < M < 20M J ) whose stellar insolation is low enough (F * < 2 × 10 8 erg s −1 cm −2 , or roughly T eff < 1000) that they are not affected by the hot Jupiter radius inflation mechanism(s). We compute a set of new thermal and structural evolution models and use these models in comparison with properties of the 47 transiting planets (… Show more

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Cited by 356 publications
(535 citation statements)
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References 100 publications
(84 reference statements)
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“…Figure 4 shows the total mass of heavy elements in the hot Jupiter (MZ ) as a function of their seed's initial injection place and time in the case of complete core erosion. The values we find are in line with the indirect retrieval method of Thorngren et al (2015). Planets forming earlier and further out in the disk have higher isolation masses and thus higher MZ 1 .…”
Section: Case: Solar Chemistrysupporting
confidence: 78%
“…Figure 4 shows the total mass of heavy elements in the hot Jupiter (MZ ) as a function of their seed's initial injection place and time in the case of complete core erosion. The values we find are in line with the indirect retrieval method of Thorngren et al (2015). Planets forming earlier and further out in the disk have higher isolation masses and thus higher MZ 1 .…”
Section: Case: Solar Chemistrysupporting
confidence: 78%
“…14). These high heavy element contents agree at least in an approximate way with the observationally inferred values (Thorngren et al 2016) as discussed in detail in Sect. 5.1.8.…”
Section: Uncertainties Related To the Core-mass Effectsupporting
confidence: 72%
“…In the solar system, the highest total heavy element content of Jupiter allowed by internal structure models is about 42 M ⊕ for adiabatic models and the SCvH EOS (Guillot & Gautier 2014), while for semi-convective models up to 63 M ⊕ are possible (Leconte & Chabrier 2012). Concerning exoplanets, thanks to recent analyses (Miller & Fortney 2011;Thorngren et al 2016) of the mass-radius relation of warm Jupiters without significant bloating, it is now possible to infer observationally estimates of the heavy element mass contained in planets also outside the solar system. While these analyses are (as those for Jupiter) affected by many uncertainties, e.g., regarding the equation of state and cannot yield (in contrast to the solar system) information about the distribution of the heavy elements within the planet (in the core or mixed throughout the envelope) they still significantly increase the number of planets with heavy element estimates and allow to make statistical inferences.…”
Section: Comparison With Observed Forming Companions: Hd 100546 B Andmentioning
confidence: 99%
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