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

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

doi:10.1007/s11214-018-0574-6

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

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

Research output: Contribution to journal › Review article › peer-review

292 Scopus citations

Abstract

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 ∼200000 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 M _w ∼ 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.

Original language	English (US)
Article number	12
Journal	Space Science Reviews
Volume	215
Issue number	1
DOIs	https://doi.org/10.1007/s11214-018-0574-6
State	Published - Jan 1 2019

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

Keywords

InSight
Mars seismology

Access to Document

10.1007/s11214-018-0574-6

Cite this

Lognonné, P., Banerdt, W. B., Giardini, D., Pike, W. T., Christensen, U., Laudet, P., de Raucourt, S., Zweifel, P., Calcutt, S., Bierwirth, M., Hurst, K. J., Ijpelaan, F., Umland, J. W., Llorca-Cejudo, R., Larson, S. A., Garcia, R. F., Kedar, S., Knapmeyer-Endrun, B., Mimoun, D., ... Wookey, J. (2019). SEIS: Insight’s Seismic Experiment for Internal Structure of Mars. Space Science Reviews, 215(1), Article 12. https://doi.org/10.1007/s11214-018-0574-6

@article{88fce7083d314670b72db953d11bef46,

title = "SEIS: Insight{\textquoteright}s Seismic Experiment for Internal Structure of Mars",

abstract = " By the end of 2018, 42 years after the landing of the two Viking seismometers on Mars, InSight will deploy onto Mars{\textquoteright} 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{\textquoteright}s Mars seismic monitoring by a factor of ∼ 2500 at 1 Hz and ∼200000 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{\textquoteright} 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 M w ∼ 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.",

keywords = "InSight, Mars seismology",

author = "P. Lognonn{\'e} and Banerdt, {W. B.} and D. Giardini and Pike, {W. T.} and U. Christensen and P. Laudet and {de Raucourt}, S. and P. Zweifel and S. Calcutt and M. Bierwirth and Hurst, {K. J.} and F. Ijpelaan and Umland, {J. W.} and R. Llorca-Cejudo and Larson, {S. A.} and Garcia, {R. F.} and S. Kedar and B. Knapmeyer-Endrun and D. Mimoun and A. Mocquet and Panning, {M. P.} and Weber, {R. C.} and A. Sylvestre-Baron and G. Pont and N. Verdier and L. Kerjean and Facto, {L. J.} and V. Gharakanian and Feldman, {J. E.} and Hoffman, {T. L.} and Klein, {D. B.} and K. Klein and Onufer, {N. P.} and J. Paredes-Garcia and Petkov, {M. P.} and Willis, {J. R.} and Smrekar, {S. E.} and M. Drilleau and T. Gabsi and T. Nebut and O. Robert and S. Tillier and C. Moreau and M. Parise and G. Aveni and {Ben Charef}, S. and Y. Bennour and T. Camus and Dandonneau, {P. A.} and C. Desfoux and B. Lecomte and O. Pot and P. Revuz and D. Mance and J. tenPierick and Bowles, {N. E.} and C. Charalambous and Delahunty, {A. K.} and J. Hurley and R. Irshad and Huafeng Liu and Mukherjee, {A. G.} and Standley, {I. M.} and Stott, {A. E.} and J. Temple and T. Warren and M. Eberhardt and A. Kramer and W. K{\"u}hne and Miettinen, {E. P.} and M. Monecke and C. Aicardi and M. Andr{\'e} and J. Baroukh and A. Borrien and A. Bouisset and P. Boutte and K. Brethom{\'e} and C. Brysbaert and T. Carlier and M. Deleuze and Desmarres, {J. M.} and D. Dilhan and C. Doucet and D. Faye and N. Faye-Refalo and R. Gonzalez and C. Imbert and C. Larigauderie and E. Locatelli and L. Luno and Meyer, {J. R.} and F. Mialhe and Mouret, {J. M.} and M. Nonon and Y. Pahn and A. Paillet and P. Pasquier and G. Perez and R. Perez and L. Perrin and B. Pouilloux and A. Rosak and {Savin de Larclause}, I. and J. Sicre and M. Sodki and N. Toulemont and B. Vella and C. Yana and F. Alibay and Avalos, {O. M.} and Balzer, {M. A.} and P. Bhandari and E. Blanco and Bone, {B. D.} and Bousman, {J. C.} and P. Bruneau and Calef, {F. J.} and Calvet, {R. J.} and D{\textquoteright}Agostino, {S. A.} and {de los Santos}, G. and Deen, {R. G.} and Denise, {R. W.} and J. Ervin and Ferraro, {N. W.} and Gengl, {H. E.} and F. Grinblat and D. Hernandez and M. Hetzel and Johnson, {M. E.} and L. Khachikyan and Lin, {J. Y.} and Madzunkov, {S. M.} and Marshall, {S. L.} and Mikellides, {I. G.} and Miller, {E. A.} and W. Raff and Singer, {J. E.} and Sunday, {C. M.} and Villalvazo, {J. F.} and Wallace, {M. C.} and D. Banfield and Rodriguez-Manfredi, {J. A.} and Russell, {C. T.} and A. Trebi-Ollennu and Maki, {J. N.} and E. Beucler and M. B{\"o}se and C. Bonjour and Berenguer, {J. L.} and S. Ceylan and J. Clinton and V. Conejero and I. Daubar and V. Dehant and P. Delage and F. Euchner and I. Est{\`e}ve and L. Fayon and L. Ferraioli and Johnson, {C. L.} and J. Gagnepain-Beyneix and M. Golombek and A. Khan and T. Kawamura and B. Kenda and P. Labrot and N. Murdoch and C. Pardo and C. Perrin and L. Pou and A. Sauron and D. Savoie and S. St{\"a}hler and E. Stutzmann and Teanby, {N. A.} and Jeroen Tromp and {van Driel}, M. and M. Wieczorek and R. Widmer-Schnidrig and J. Wookey",

note = "Publisher Copyright: {\textcopyright} 2019, The Author(s).",

year = "2019",

month = jan,

day = "1",

doi = "10.1007/s11214-018-0574-6",

language = "English (US)",

volume = "215",

journal = "Space Science Reviews",

issn = "0038-6308",

publisher = "Springer Netherlands",

number = "1",

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Lognonné, P, Banerdt, WB, Giardini, D, Pike, WT, Christensen, U, Laudet, P, de Raucourt, S, Zweifel, P, Calcutt, S, Bierwirth, M, Hurst, KJ, Ijpelaan, F, Umland, JW, Llorca-Cejudo, R, Larson, SA, Garcia, RF, Kedar, S, Knapmeyer-Endrun, B, Mimoun, D, Mocquet, A, Panning, MP, Weber, RC, Sylvestre-Baron, A, Pont, G, Verdier, N, Kerjean, L, Facto, LJ, Gharakanian, V, Feldman, JE, Hoffman, TL, Klein, DB, Klein, K, Onufer, NP, Paredes-Garcia, J, Petkov, MP, Willis, JR, Smrekar, SE, Drilleau, M, Gabsi, T, Nebut, T, Robert, O, Tillier, S, Moreau, C, Parise, M, Aveni, G, Ben Charef, S, Bennour, Y, Camus, T, Dandonneau, PA, Desfoux, C, Lecomte, B, Pot, O, Revuz, P, Mance, D, tenPierick, J, Bowles, NE, Charalambous, C, Delahunty, AK, Hurley, J, Irshad, R, Liu, H, Mukherjee, AG, Standley, IM, Stott, AE, Temple, J, Warren, T, Eberhardt, M, Kramer, A, Kühne, W, Miettinen, EP, Monecke, M, Aicardi, C, André, M, Baroukh, J, Borrien, A, Bouisset, A, Boutte, P, Brethomé, K, Brysbaert, C, Carlier, T, Deleuze, M, Desmarres, JM, Dilhan, D, Doucet, C, Faye, D, Faye-Refalo, N, Gonzalez, R, Imbert, C, Larigauderie, C, Locatelli, E, Luno, L, Meyer, JR, Mialhe, F, Mouret, JM, Nonon, M, Pahn, Y, Paillet, A, Pasquier, P, Perez, G, Perez, R, Perrin, L, Pouilloux, B, Rosak, A, Savin de Larclause, I, Sicre, J, Sodki, M, Toulemont, N, Vella, B, Yana, C, Alibay, F, Avalos, OM, Balzer, MA, Bhandari, P, Blanco, E, Bone, BD, Bousman, JC, Bruneau, P, Calef, FJ, Calvet, RJ, D’Agostino, SA, de los Santos, G, Deen, RG, Denise, RW, Ervin, J, Ferraro, NW, Gengl, HE, Grinblat, F, Hernandez, D, Hetzel, M, Johnson, ME, Khachikyan, L, Lin, JY, Madzunkov, SM, Marshall, SL, Mikellides, IG, Miller, EA, Raff, W, Singer, JE, Sunday, CM, Villalvazo, JF, Wallace, MC, Banfield, D, Rodriguez-Manfredi, JA, Russell, CT, Trebi-Ollennu, A, Maki, JN, Beucler, E, Böse, M, Bonjour, C, Berenguer, JL, Ceylan, S, Clinton, J, Conejero, V, Daubar, I, Dehant, V, Delage, P, Euchner, F, Estève, I, Fayon, L, Ferraioli, L, Johnson, CL, Gagnepain-Beyneix, J, Golombek, M, Khan, A, Kawamura, T, Kenda, B, Labrot, P, Murdoch, N, Pardo, C, Perrin, C, Pou, L, Sauron, A, Savoie, D, Stähler, S, Stutzmann, E, Teanby, NA, Tromp, J, van Driel, M, Wieczorek, M, Widmer-Schnidrig, R & Wookey, J 2019, 'SEIS: Insight’s Seismic Experiment for Internal Structure of Mars', Space Science Reviews, vol. 215, no. 1, 12. https://doi.org/10.1007/s11214-018-0574-6

TY - JOUR

T1 - SEIS

T2 - Insight’s Seismic Experiment for Internal Structure of Mars

AU - Lognonné, P.

AU - Banerdt, W. B.

AU - Giardini, D.

AU - Pike, W. T.

AU - Christensen, U.

AU - Laudet, P.

AU - de Raucourt, S.

AU - Zweifel, P.

AU - Calcutt, S.

AU - Bierwirth, M.

AU - Hurst, K. J.

AU - Ijpelaan, F.

AU - Umland, J. W.

AU - Llorca-Cejudo, R.

AU - Larson, S. A.

AU - Garcia, R. F.

AU - Kedar, S.

AU - Knapmeyer-Endrun, B.

AU - Mimoun, D.

AU - Mocquet, A.

AU - Panning, M. P.

AU - Weber, R. C.

AU - Sylvestre-Baron, A.

AU - Pont, G.

AU - Verdier, N.

AU - Kerjean, L.

AU - Facto, L. J.

AU - Gharakanian, V.

AU - Feldman, J. E.

AU - Hoffman, T. L.

AU - Klein, D. B.

AU - Klein, K.

AU - Onufer, N. P.

AU - Paredes-Garcia, J.

AU - Petkov, M. P.

AU - Willis, J. R.

AU - Smrekar, S. E.

AU - Drilleau, M.

AU - Gabsi, T.

AU - Nebut, T.

AU - Robert, O.

AU - Tillier, S.

AU - Moreau, C.

AU - Parise, M.

AU - Aveni, G.

AU - Ben Charef, S.

AU - Bennour, Y.

AU - Camus, T.

AU - Dandonneau, P. A.

AU - Desfoux, C.

AU - Lecomte, B.

AU - Pot, O.

AU - Revuz, P.

AU - Mance, D.

AU - tenPierick, J.

AU - Bowles, N. E.

AU - Charalambous, C.

AU - Delahunty, A. K.

AU - Hurley, J.

AU - Irshad, R.

AU - Liu, Huafeng

AU - Mukherjee, A. G.

AU - Standley, I. M.

AU - Stott, A. E.

AU - Temple, J.

AU - Warren, T.

AU - Eberhardt, M.

AU - Kramer, A.

AU - Kühne, W.

AU - Miettinen, E. P.

AU - Monecke, M.

AU - Aicardi, C.

AU - André, M.

AU - Baroukh, J.

AU - Borrien, A.

AU - Bouisset, A.

AU - Boutte, P.

AU - Brethomé, K.

AU - Brysbaert, C.

AU - Carlier, T.

AU - Deleuze, M.

AU - Desmarres, J. M.

AU - Dilhan, D.

AU - Doucet, C.

AU - Faye, D.

AU - Faye-Refalo, N.

AU - Gonzalez, R.

AU - Imbert, C.

AU - Larigauderie, C.

AU - Locatelli, E.

AU - Luno, L.

AU - Meyer, J. R.

AU - Mialhe, F.

AU - Mouret, J. M.

AU - Nonon, M.

AU - Pahn, Y.

AU - Paillet, A.

AU - Pasquier, P.

AU - Perez, G.

AU - Perez, R.

AU - Perrin, L.

AU - Pouilloux, B.

AU - Rosak, A.

AU - Savin de Larclause, I.

AU - Sicre, J.

AU - Sodki, M.

AU - Toulemont, N.

AU - Vella, B.

AU - Yana, C.

AU - Alibay, F.

AU - Avalos, O. M.

AU - Balzer, M. A.

AU - Bhandari, P.

AU - Blanco, E.

AU - Bone, B. D.

AU - Bousman, J. C.

AU - Bruneau, P.

AU - Calef, F. J.

AU - Calvet, R. J.

AU - D’Agostino, S. A.

AU - de los Santos, G.

AU - Deen, R. G.

AU - Denise, R. W.

AU - Ervin, J.

AU - Ferraro, N. W.

AU - Gengl, H. E.

AU - Grinblat, F.

AU - Hernandez, D.

AU - Hetzel, M.

AU - Johnson, M. E.

AU - Khachikyan, L.

AU - Lin, J. Y.

AU - Madzunkov, S. M.

AU - Marshall, S. L.

AU - Mikellides, I. G.

AU - Miller, E. A.

AU - Raff, W.

AU - Singer, J. E.

AU - Sunday, C. M.

AU - Villalvazo, J. F.

AU - Wallace, M. C.

AU - Banfield, D.

AU - Rodriguez-Manfredi, J. A.

AU - Russell, C. T.

AU - Trebi-Ollennu, A.

AU - Maki, J. N.

AU - Beucler, E.

AU - Böse, M.

AU - Bonjour, C.

AU - Berenguer, J. L.

AU - Ceylan, S.

AU - Clinton, J.

AU - Conejero, V.

AU - Daubar, I.

AU - Dehant, V.

AU - Delage, P.

AU - Euchner, F.

AU - Estève, I.

AU - Fayon, L.

AU - Ferraioli, L.

AU - Johnson, C. L.

AU - Gagnepain-Beyneix, J.

AU - Golombek, M.

AU - Khan, A.

AU - Kawamura, T.

AU - Kenda, B.

AU - Labrot, P.

AU - Murdoch, N.

AU - Pardo, C.

AU - Perrin, C.

AU - Pou, L.

AU - Sauron, A.

AU - Savoie, D.

AU - Stähler, S.

AU - Stutzmann, E.

AU - Teanby, N. A.

AU - Tromp, Jeroen

AU - van Driel, M.

AU - Wieczorek, M.

AU - Widmer-Schnidrig, R.

AU - Wookey, J.

PY - 2019/1/1

Y1 - 2019/1/1

N2 - 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 ∼200000 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 M w ∼ 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.

AB - 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 ∼200000 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 M w ∼ 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.

KW - InSight

KW - Mars seismology

UR - http://www.scopus.com/inward/record.url?scp=85060754712&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=85060754712&partnerID=8YFLogxK

U2 - 10.1007/s11214-018-0574-6

DO - 10.1007/s11214-018-0574-6

M3 - Review article

C2 - 30880848

AN - SCOPUS:85060754712

SN - 0038-6308

VL - 215

JO - Space Science Reviews

JF - Space Science Reviews

IS - 1

M1 - 12

ER -

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

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