000005872 001__ 5872
000005872 005__ 20221028113011.0
000005872 0247_ $$2DOI$$a10.1073/pnas.2204474119
000005872 037__ $$aSCART-2022-0104
000005872 100__ $$aHuang, Quancheng 
000005872 245__ $$aSeismic detection of a deep mantle discontinuity within Mars by InSight
000005872 260__ $$c2022
000005872 520__ $$aConstraining the thermal and compositional state of the mantle is crucial for deciphering the formation and evolution of Mars. Mineral physics predicts that Mars? deep mantle is demarcated by a seismic discontinuity arising from the pressure-induced phase transformation of the mineral olivine to its higher-pressure polymorphs, making the depth of this boundary sensitive to both mantle temperature and composition. Here, we report on the seismic detection of a midmantle discontinuity using the data collected by NASA?s InSight Mission to Mars that matches the expected depth and sharpness of the postolivine transition. In five teleseismic events, we observed triplicated P and S waves and constrained the depth of this discontinuity to be 1,006 $\pm$40 km by modeling the triplicated waveforms. From this depth range, we infer a mantle potential temperature of 1,605 $\pm$100 K, a result consistent with a crust that is 10 to 15 times more enriched in heat-producing elements than the underlying mantle. Our waveform fits to the data indicate a broad gradient across the boundary, implying that the Martian mantle is more enriched in iron compared to Earth. Through modeling of thermochemical evolution of Mars, we observe that only two out of the five proposed composition models are compatible with the observed boundary depth. Our geodynamic simulations suggest that the Martian mantle was relatively cold 4.5 Gyr ago (1,720 to 1,860 K) and are consistent with a present-day surface heat flow of 21 to 24 mW/m2.
000005872 536__ $$a3PRPDPLANINT/$$c3PRPDPLANINT/$$f3PRPDPLANINT
000005872 594__ $$aNO
000005872 700__ $$aSchmerr, Nicholas C. 
000005872 700__ $$aKing, Scott D. 
000005872 700__ $$aKim, Doyeon 
000005872 700__ $$aRivoldini, Attilio 
000005872 700__ $$aPlesa, Ana-Catalina 
000005872 700__ $$aSamuel, Henri 
000005872 700__ $$aMaguire, Ross R. 
000005872 700__ $$aKarakostas, Foivos 
000005872 700__ $$aLekić, Vedran 
000005872 700__ $$aCharalambous, Constantinos 
000005872 700__ $$aCollinet, Max 
000005872 700__ $$aMyhill, Robert 
000005872 700__ $$aAntonangeli, Daniele 
000005872 700__ $$aDrilleau, Mélanie 
000005872 700__ $$aBystricky, Misha 
000005872 700__ $$aBollinger, Caroline 
000005872 700__ $$aMichaut, Chloé 
000005872 700__ $$aGudkova, Tamara 
000005872 700__ $$aIrving, Jessica C. E. 
000005872 700__ $$aHorleston, Anna 
000005872 700__ $$aFernando, Benjamin 
000005872 700__ $$aLeng, Kuangdai 
000005872 700__ $$aNissen-Meyer, Tarje 
000005872 700__ $$aBejina, Frederic 
000005872 700__ $$aBozdağ, Ebru 
000005872 700__ $$aBeghein, Caroline 
000005872 700__ $$aWaszek, Lauren 
000005872 700__ $$aSiersch, Nicki C. 
000005872 700__ $$aScholz, John-Robert 
000005872 700__ $$aDavis, Paul M. 
000005872 700__ $$aLognonné, Philippe 
000005872 700__ $$aPinot, Baptiste 
000005872 700__ $$aWidmer-Schnidrig, Rudolf 
000005872 700__ $$aPanning, Mark P. 
000005872 700__ $$aSmrekar, Suzanne E. 
000005872 700__ $$aSpohn, Tilman 
000005872 700__ $$aPike, William T. 
000005872 700__ $$aGiardini, Domenico 
000005872 700__ $$aBanerdt, W. Bruce
000005872 773__ $$n42$$pProceedings of the National Academy of Sciences$$v119$$y2022
000005872 8560_ $$fattilio.rivoldini@observatoire.be
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000005872 905__ $$apublished in
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