Publication date: Jul 13, 2020
The impact of the inner structure and thermal history of planets on their observable features, such as luminosity or magnetic field, crucially depends on the poorly known heat and charge transport properties of their internal layers. The thermal and electric conductivities of different phases of water (liquid, solid, and super-ionic) occurring in the interior of ice giant planets, such as Uranus or Neptune, are evaluated from equilibrium ab initio molecular dynamics, leveraging recent progresses in the theory and data analysis of transport in extended systems. In this record we collect the ab-initio time series of the energy flux and of the electronic and ionic charge fluxes for H2O at different planetary conditions, from which the related transport coefficients are extracted according to the Green-Kubo theory of linear response.
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|81.2 MiB||Contains the time series of heat and charge fluxes, as well as a minimal PDF guide on how to analyse the timeseries via the GUI version of the Thermocepstrum code.|
|268.3 KiB||Contains the time series of energy bandgap of two simulation of superionic water and a Jupyter notebook to plot the results.|
|39.4 MiB||Contains the thermocepstrum + GUI code version with which the GUI-oriented files *_thermocepstrum.npy were saved.|
|923 Bytes||README file with descriptions on the contents of the different directories.|