000005259 001__ 5259
000005259 005__ 20210201174842.0
000005259 037__ $$aPOSTER-2021-0018
000005259 100__ $$aPlesa, Ana-Catalina 
000005259 245__ $$aSeismic Velocities Distribution in a 3D Mantle: Implications for InSight Measurements
000005259 260__ $$c2020
000005259 269__ $$c2020-12-15
000005259 520__ $$aThe InSight mission [1] landed in November 2018 in the Elysium Planitia region [2] bringing the first geophysical observatory to Mars. Since February 2019 the seismometer SEIS [3] has continuously recorded Mars' seismic activity, and a list of the seismic events is available in the InSight Marsquake Service catalog [4]. In this study, we predict present-day seismic velocities in the Martian interior using the 3D thermal evolution models of [5] (Fig. 1a, b). We then use the 3D velocity distributions to interpret seismic observations recorded by InSight. Our analysis is focused on the two high quality events S0173a and S0235b. Both have distinguishable P- and S-wave arrivals and are thought to originate in Cerberus Fossae [6], a potentially active fault system [7]. Our results show that models with a crust containing more than half of the total amount of heat producing elements (HPE) of the bulk of Mars lead to large variations of the seismic velocities in the lithosphere. A seismic velocity pattern similar to the crustal thickness structure is observed at depths larger than 400 km for cases with cold and thick lithospheres. Models, with less than 20% of the total HPE in the crust have thinner lithospheres with shallower but more prominent low velocity zones. The latter, lead to shadow zones that are incompatible with the observed P- and S-wave arrivals of seismic events occurring in Cerberus Fossae, in 20° - 40° epicentral distance (Fig. 1c). We therefore expect that future high-quality seismic events have the potential to further constrain the amount of HPE in the Martian crust. Future work will combine the seismic velocities distribution calculated in this study with modeling of seismic wave propagation [8, 9] (Fig. 1d). This will help to assess the effects of a 3D thermal structure on the waveforms and provide a powerful framework for the interpretation of InSight’s seismic data.
000005259 594__ $$aNO
000005259 700__ $$aBozdag, Ebru
000005259 700__ $$aRivoldini, Attilio
000005259 700__ $$aKnapmeyer, Martin
000005259 700__ $$aMcLennan, Scott
000005259 700__ $$aPadovan, Sebastiano
000005259 700__ $$aTosi, Nicola
000005259 700__ $$aBreuer, Doris
000005259 700__ $$aPeter, Daniel
000005259 700__ $$aStaehler, Simon
000005259 700__ $$aWieczorek, Mark
000005259 700__ $$avan Driel, Martin
000005259 700__ $$aKhan, Amir
000005259 700__ $$aSpohn, Tilman
000005259 700__ $$aCiardelli, Caio
000005259 700__ $$aKing, Scott
000005259 773__ $$tAGU Fall Meeting 2020, Virtual
000005259 8560_ $$fattilio.rivoldini@observatoire.be
000005259 85642 $$ahttps://agu.confex.com/agu/fm20/meetingapp.cgi/Paper/726609
000005259 980__ $$aCPOSTER