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Simulations, Data Analysis and Algorithms

Computational Astrophysics and Cosmology Cover Image
Figure 1 | Computational Astrophysics and Cosmology

Figure 1

From: Machine learning applied to simulations of collisions between rotating, differentiated planets

Figure 1

Cross-section of a model. The top panel shows the cross-section of a model in its non-rotating state as generated by ballic. In the bottom panel, a cross-section of that same model is shown in its rotating state after being spun-up by Gasoline. The model shown in this figure is designated YRMmYF in the 12D_LHS200 dataset and has the following properties: \(M = 1.192~\mathrm{M}_{\oplus }\), \(F^{\mathrm{core}}_{\mathrm{body}} = 0.122\), \(\Omega = 0.869~\Omega _{\mathrm{crit}}\), \(\epsilon _{\mathrm{body}} = 0.486\), and \(\epsilon _{\mathrm{core}} = 0.2966\), where ϵ is the flattening. Note that the flattening of the core is less than that of the entire body

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