Bonding and electronic properties of ice at high pressure

Militzer, Burkhard

doi:10.1002/qua.23247

Cited by 1 publication

(1 citation statement)

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“…Recent molecular dynamics simulations (Cavazzoni 1999, Militzer & Wilson 2010, Militzer 2012, Hermann et al 2011, Wang et al 2011) have predicted multiple new phases of ice at P 10 11 Pa. In particular, ice is likely in either a superionic or fluid phase at the core conditions of Saturn , Wilson & Militzer 2012, depending on the core temperature.…”

Section: The Shear Modulusmentioning

confidence: 99%

Non-radial oscillations in rotating giant planets with solid cores: Application to Saturn and its rings

Fuller

Lai

Storch

2014

Icarus

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Recent observations have revealed evidence for the global acoustic oscillations of Jupiter and Saturn. Such oscillations can potentially provide a new window into the interior structure of giant planets. Motivated by these observations, we study the non-radial oscillation modes of giant planets containing a solid core. Our calculations include the elastic response of the core and consider a wide range of possible values of the core shear modulus. While the elasticity of the core only slightly changes the frequencies of acoustic modes (including the f-modes), which reside mostly in the fluid envelope, it adds two new classes of shear modes that are largely confined to the core. We also calculate the effects of the Coriolis force on the planetary oscillation modes. In addition to changing the mode frequencies, the Coriolis force can cause the shear modes to mix with the f-modes. Such mixing occurs when the frequencies of the shear mode and the f-mode are close to each other, and results in "mixed modes" that have similarly large surface displacements and gravitational potential perturbations, but are slightly split in frequency. We discuss our results in light of the recent work by Hedman & Nicholson (2013), which revealed the presence of density waves in Saturn's C-ring that appear to be excited by the gravitational perturbations associated with the f-mode oscillations within Saturn. We find that the fine splitting in wave frequencies observed in the rings can in principle be explained by the rotation-induced mixing between core shear modes and f-modes, possibly indicating the presence of a solid core within Saturn. However, in our current calculations, which assume rigid-body rotation and include only first-order rotational effects, significant fine-tuning in the planetary model parameters is needed in order to achieve these mode mixings and to explain the observed fine frequency splitting. We briefly discuss other effects that may modify the f-modes and facilitate mode mixing.

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Section: The Shear Modulusmentioning

confidence: 99%