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SEIS: Insight’s Seismic Experiment for Internal Structure of Mars

Lognonné, Philippe and Banerdt, W. Bruce and Giardini, D. and Pike, W. T. and Christensen, U. and Laudet, P. and de Raucourt, S. and Zweifel, P. and Calcutt, S. and Bierwirth, M. and Hurst, K. J. and Ijpelaan, F. and Umland, J. W. and Llorca-Cejudo, R. and Larson, S. A. and Garcia, Raphaël F. and Kedar, S. and Knapmeyer-Endrun, B. and Mimoun, David and Mocquet, A. and Panning, M. P. and Weber, R. C. and Sylvestre-Baron, A. and Pont, G. and Verdier, N. and Kerjean, L. and Facto, L. J. and Gharakanian, V. and Feldman, J. E. and Hoffman, T. L. and Klein, D. B. and Klein, K. and Onufer, N. P. and Paredes-Garcia, J. and Petkov, M. P. and Willis, J. R. and Smrekar, S. E. and Drilleau, Mélanie and Gabsi, T. and Nebut, T. and Robert, O. and Tillier, S. and Moreau, C. and Parise, M. and Aveni, G. and Ben Charef, S. and Bennour, Y. and Camus, T. and Dandonneau, P. A. and Desfoux, C. and Lecomte, B. and Pot, O. and Revuz, P. and Mance, D. and tenPierick, J. and Bowles, N. E. and Charalambous, C. and Delahunty, A. K. and Hurley, J. and Irshad, R. and Liu, Huafeng and Mukherjee, A. G. and Standley, I. M. and Stott, A. E. and Temple, J. and Warren, T. and Eberhardt, M. and Kramer, A. and Kühne, W. and Miettinen, E.-P. and Monecke, M. and Aicardi, C. and André, M. and Baroukh, J. and Borrien, A. and Bouisset, A. and Boutte, P. and Brethomé, K. and Brysbaert, C. and Carlier, T. and Deleuze, M. and Desmarres, J. M. and Dilhan, D. and Doucet, C. and Faye, D. and Faye-Refalo, N. and Gonzalez, R. and Imbert, C. and Larigauderie, C. and Locatelli, E. and Luno, L. and Meyer, J.-R. and Mialhe, F. and Mouret, J. M. and Nonon, M. and Pahn, Y. and Paillet, A. and Pasquier, P. and Perez, G. and Perez, R. and Perrin, L. and Pouilloux, B. and Rosak, A. and Savin de Larclause, I. and Sicre, J. and Sodki, M. and Toulemont, N. and Vella, B. and Yana, C. and Alibay, F. and Avalos, O. M. and Balzer, M. A. and Bhandari, P. and Blanco, E. and Bone, B. D. and Bousman, J. C. and Bruneau, P. and Calef, F. J. and Calvet, R. J. and D’Agostino, S. A. and de los Santos, G. and Deen, R. G. and Denise, R. W. and Ervin, J. and Ferraro, N. W. and Gengl, H. E. and Grinblat, F. and Hernandez, D. and Hetzel, M. and Johnson, M. E. and Khachikyan, L. and Lin, J. Y. and Madzunkov, S. M. and Marshall, S. L. and Mikellides, I. G. and Miller, E. A. and Raff, W. and Singer, J. E. and Sunday, C. M. and Villalvazo, J. F. and Wallace, M. C. and Banfield, D. and Rodriguez-Manfredi, J. A. and Russell, C. T. and Trebi-Ollennu, A. and Maki, J. N. and Beucler, E. and Böse, M. and Bonjour, C. and Berenguer, J. L. and Ceylan, S. and Clinton, J. and Conejero, V. and Daubar, I. and Dehant, V. and Delage, P. and Euchner, F. and Estève, I. and Fayon, L. and Ferraioli, L. and Johnson, C. L. and Gagnepain-Beyneix, J. and Golombek, M. and Khan, A. and Kawamura, T. and Kenda, B. and Labrot, P. and Murdoch, Naomi and Pardo, C. and Perrin, C. and Pou, L. and Sauron, A. and Savoie, D. and Stähler, S. and Stutzmann, E. and Teanby, N. A. and Tromp, J. and van Driel, M. and Wieczorek, M. and Widmer-Schnidrig, R. and Wookey, J. SEIS: Insight’s Seismic Experiment for Internal Structure of Mars. (2019) Space Science Reviews, 215 (1). 1-170. ISSN 0038-6308

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Official URL: https://doi.org/10.1007/S11214-018-0574-6


By the end of 2018, 42 years after the landing of the two Viking seismometers on Mars, InSight will deploy onto Mars’ surface the SEIS (Seismic Experiment for Internal Structure) instrument; a six-axes seismometer equipped with both a long-period three-axes Very Broad Band (VBB) instrument and a three-axes short-period (SP) instrument. These six sensors will cover a broad range of the seismic bandwidth, from 0.01 Hz to 50 Hz, with possible extension to longer periods. Data will be transmitted in the form of three continuous VBB components at 2 sample per second (sps), an estimation of the short period energy content from the SP at 1 sps and a continuous compound VBB/SP vertical axis at 10 sps. The continuous streams will be augmented by requested event data with sample rates from 20 to 100 sps. SEIS will improve upon the existing resolution of Viking’s Mars seismic monitoring by a factor of ∼ 2500 at 1 Hz and ∼ 200 000 at 0.1 Hz. An additional major improvement is that, contrary to Viking, the seismometers will be deployed via a robotic arm directly onto Mars’ surface and will be protected against temperature and wind by highly efficient thermal and wind shielding. Based on existing knowledge of Mars, it is reasonable to infer a moment magnitude detection threshold of Mw ∼ 3 at 40◦ epicentral distance and a potential to detect several tens of quakes and about five impacts per year. In this paper, we first describe the science goals of the experiment and the rationale used to define its requirements. We then provide a detailed description of the hardware, from the sensors to the deployment system and associated performance, including transfer functions of the seismic sensors and temperature sensors. We conclude by describing the experiment ground segment, including data processing services, outreach and education networks and provide a description of the format to be used for future data distribution.

Item Type:Article
HAL Id:hal-02873390
Audience (journal):International peer-reviewed journal
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Institution:Université de Toulouse > Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE)
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Deposited On:18 Jun 2020 09:36

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