Fig. 2: Summary of Mars’s interior structure. | Nature

Fig. 2: Summary of Mars’s interior structure.

From: Evidence for a liquid silicate layer atop the Martian core

Fig. 2

a, Inverted S- and P-wave velocity and density profiles. For comparison, black solid and dashed lines represent the range of core profiles determined previously using seismic core-transiting (SKS) data2. b, Body wave ray path geometry for all events (labelled with stars) considered in this study. Colour bar denotes ray path density, that is, the number of rays passing through a given area, based on the inverted models shown in a, which explains the diffuseness of the ray paths and source locations. The horizontal column below ‘InSight’ is the radial sensitivity and computed as the integrated ray path density with epicentral distance. Note that the SKS phase for event S0976a is only predicted and not inverted (see Supplementary Information section 1 for details). c, Inverted molten silicate layer (LSL) properties (in blue): mean density (\({\bar{\rho }}_{{\rm{LSL}}}\)), mean P-wave velocity (\({\bar{V}}_{{\rm{P}}}^{{\rm{LSL}}}\)) and thickness (ΔZ). d, Inverted core properties (in blue): mean density (\({\bar{\rho }}_{{\rm{core}}}\)) and core radius (Rcore). The probability contours shown in orange in c and d have been obtained by downsampling the models to additionally match the observed diffracted P-wave reverberation (\({{{\rm{P}}}_{{\rm{d}}{\rm{i}}{\rm{f}}{\rm{f}}}}^{\hat{}}{\rm{L}}{\rm{S}}{\rm{L}}\,{{\rm{P}}}_{{\rm{d}}{\rm{i}}{\rm{f}}{\rm{f}}}\)) in the LSL (see Fig. 3c and main text for details). Blue- and orange-shaded distributions on top and to the right of c and d indicate sampled probability distributions for the various parameters shown in the plots.

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