Core Sizes and Internal Structure of Earth's and Jupiter's Satellites

Kuskov, O. L.; Kronrod, V. A.

doi:10.1006/icar.2001.6611

Cited by 100 publications

(47 citation statements)

References 114 publications

(206 reference statements)

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“…This value together with the mass of the planet suggests a core radius of 220 km to 450 km. This range is consistent with independent lunar electromagnetic induction data (Hood et al 1999) and joint inversions of seismic and gravity data (e.g., Khan et al 2004) and with the chemical models of Kuskov and Kronrod (2001). The densities consistent with the radii given above vary between roughly 5100 kg m −3 and 8100 kg m −3 .…”

Section: Structure Sets the Stagesupporting

confidence: 68%

Thermal Evolution and Magnetic Field Generation in Terrestrial Planets and Satellites

Breuer¹,

Labrosse²,

Spohn³

2010

Space Sci Rev

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Of the terrestrial planets, Earth and Mercury have self-sustained fields while Mars and Venus do not. Magnetic field data recorded at Ganymede have been interpreted as evidence of a self-generated magnetic field. The other icy Galilean satellites have magnetic fields induced in their subsurface oceans while Io and the Saturnian satellite Titan apparently are lacking magnetic fields of internal origin altogether.

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Section: Structure Sets the Stagesupporting

confidence: 68%

Thermal Evolution and Magnetic Field Generation in Terrestrial Planets and Satellites

Breuer¹,

Labrosse²,

Spohn³

2010

Space Sci Rev

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“…Associated uncertainties are very different depending on data and model assumptions. For example, core radius R c of the Moon, Mars and Mercury, is estimated to be 310−320 km (Kuskov & Kronrod 2001), 1680 ± 150 km (Khan & Connolly 2008), and 2020 ± 100 (Padovan et al 2014), respectively.…”

Section: Solar System Planetsmentioning

confidence: 99%

Can we constrain the interior structure of rocky exoplanets from mass and radius measurements?

Dorn

Khan

Heng

et al. 2015

A&A

285

355

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Aims. We present an inversion method based on Bayesian analysis to constrain the interior structure of terrestrial exoplanets, in the form of chemical composition of the mantle and core size. Specifically, we identify what parts of the interior structure of terrestrial exoplanets can be determined from observations of mass, radius, and stellar elemental abundances. Methods. We perform a full probabilistic inverse analysis to formally account for observational and model uncertainties and obtain confidence regions of interior structure models. This enables us to characterize how model variability depends on data and associated uncertainties. Results. We test our method on terrestrial solar system planets and find that our model predictions are consistent with independent estimates. Furthermore, we apply our method to synthetic exoplanets up to 10 Earth masses and up to 1.7 Earth radii, and to exoplanet Kepler-36b. Importantly, the inversion strategy proposed here provides a framework for understanding the level of precision required to characterize the interior of exoplanets. Conclusions. Our main conclusions are (1) observations of mass and radius are sufficient to constrain core size; (2) stellar elemental abundances (Fe, Si, Mg) are principal constraints to reduce degeneracy in interior structure models and to constrain mantle composition; (3) the inherent degeneracy in determining interior structure from mass and radius observations does not only depend on measurement accuracies, but also on the actual size and density of the exoplanet. We argue that precise observations of stellar elemental abundances are central in order to place constraints on planetary bulk composition and to reduce model degeneracy. We provide a general methodology of analyzing interior structures of exoplanets that may help to understand how interior models are distributed among star systems. The methodology we propose is sufficiently general to allow its future extension to more complex internal structures including hydrogen-and water-rich exoplanets.

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“…Anderson et al, 1996Anderson et al, , 1998Kuskov and Kronrod, 2001;Sohl et al, 2002). Proposals for the accretion and differentiation of these bodies suggest that the ice, silicate and iron-dominated portions of the bodies, although segregated currently, interacted over a large range of pressure and temperature in the past (Scott et al, 2002).…”

Section: Planetary Implicationsmentioning

confidence: 99%