First Receiver Functions on Mars - Constraints on the Martian Crust from InSight

Page: Submitter Information First Name Brigitte First Middle Initial Second Middle Initial Last Name Knapmeyer-Endrun Email Address [email protected] Mobile Phone Number +49 160 8850969 Institution Name Bensberg Observatory, University of Cologne City Cologne Country Germany State / Province Student Presentation No Page: Author Information Submission: 5387 First Receiver Functions on Mars – Constraints on the Martian Crust from InSight Started at: 1/14/2020 07:02 AM - Finalized at: 1/14/2020 07:46 AM Brigitte Knapmeyer-Endrun Presenting Author Corresponding Author [email protected] Bensberg Observatory, University of Cologne, Cologne, Germany Felix Bissig [email protected] ETH Zuerich, Zuerich, Switzerland Nicolas Compaire [email protected] ISAE SUPAERO, Toulouse, France Rakshit Joshi [email protected] Max Planck Institute for Solar System Research, Göttingen, Germany Raphael Garcia [email protected] ISAE SUPAERO, Toulouse, France Amir Khan [email protected] ETH Zuerich, Zuerich, Switzerland Doyeon Kim [email protected] University of Maryland, College Park, Maryland, United States Vedran Lekić [email protected] University of Maryland, College Park, Maryland, United States Ludovic Margerin [email protected] Institut de Recherche en Astrophysique et Planetologie, Toulouse, France Mark P Panning [email protected] Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, United States Martin Schimmel [email protected] Instituto de Ciencias de la Tierra Jaume Almera, Barcelona, Spain Nicholas C Schmerr [email protected] University of Maryland, College Park, Maryland, United States Eléonore Stutzmann [email protected] Institute de Physique du Globe de Paris, Paris, France Benoit Tauzin [email protected] Universite de Lyon, Lyon, France Saikiran Tharimena [email protected] Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, United States Ebru H Bozdağ [email protected] Colorado School of Mines, Golden, Colorado, United States Daniel B Peter [email protected] KAUST, Jeddah, Saudi Arabia Ana-Catalina Plesa [email protected] DLR, Berlin, Germany Paul M Davis [email protected] University of California Los Angeles, Los Angeles, California, United States Baptiste Pinot [email protected] ISAE SUPAERO, Toulouse, France John-Robert Scholz [email protected] Max Planck Institute for Solar System Research, Göttingen, Germany Simon C Stähler [email protected] ETH Zuerich, Zuerich, Switzerland Daniele Antonangeli [email protected] Sorbonne Université, Paris, France Lu Pan [email protected] Université de Lyon, Lyon, France Clément Perrin [email protected] Institute de Physique du Globe de Paris, Paris, France Mark Wieczorek [email protected] Observatoire de la Côte d'Azur, Nice, France Philippe Lognonné [email protected] Institute de Physique du Globe de Paris, Paris, France Domenico Giardini [email protected] ETH Zuerich, Zuerich, Switzerland Suzanne E Smrekar [email protected] Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, United States William B Banerdt [email protected] Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, United States Page: Abstract Information Abstract Title First Receiver Functions on Mars – Constraints on the Martian Crust from InSight Abstract Description NASA’s InSight mission has for the first time deployed a very broad-band seismometer, SEIS, on the surface of Mars, which has been collecting data continuously since early February 2019. The main focus of InSight is to enhance our understanding of the internal structure and dynamics of Mars, including better constraints on its crustal thickness. Various models based on topography and gravity observed from the orbit currently differ by more than 100% for the average crustal thickness. Here, we present P-to-S and S-to-P receiver functions, which are available for 4 and 3 marsquakes, respectively, up to now. All of these quakes are located at comparatively small epicentral distances, between 25° and 40°. We observe three consistent phases within the first 10 seconds of the P-to-S receiver functions. The S-to-P receiver functions also show a consistent first phase. Later arrivals are harder to pinpoint, which could be due to the comparatively shallow incidence of the S-waves at the considered distances, which prevents the generation of converted waves. To obtain better constraints on velocity, we also calculated apparent velocity curves from the P-to-S receiver functions, but these provide meaningful results for only one event so far, implying a large uncertainty. Due to difficulties in clearly identifying multiples, the receiver functions can currently be explained by either two crustal layers and a thin (25-30 km) crust or three crustal layers and a thicker (40-45 km) crust at the landing site. This model range already improves the present constraints by providing a new maximum value of less than 70 km instead of more than 100 km for the average crustal thickness. Information from noise autocorrelations as a complementary method, identification of P-reverberations and Sprecursors in the event recordings, and more extensive modeling, ultimately including 3D-effects, are investigated to tighten the constraints. Page: Technical Sessions Technical Session Insight Seismology on Mars: Results From the First (Earth) Year of Data and Prospects for the Future Presentation Preference Oral Are you the abstract presenting author? Yes SSA will be recording presentations at the 2019 Annual Meeting. As the presenting author, does SSA have your permission to publish a video, audio or image file of your presentation on the SSA website? No