Examinando por Autor "Lorenz, R."

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A Study of Daytime Convective Vortices and Turbulence in the Martian Planetary Boundary Layer Based on Half-a-Year of InSight Atmospheric Measurements and Large-Eddy Simulations
(American Geophysical Union: Advancing Earth and Space Science, 2021-01-12) Spiga, A.; Murdoch, N.; Lorenz, R.; Forget, F.; Newman, C. E.; Rodríguez, Sébastien; Pla García, J.; Viúdez Moreiras, Daniel; Banfield, D.; Perrin, C.; Mueller, N. T.; Lemmon, M. T.; Millour, E.; Banerdt, W. B.; Agencia Estatal de Investigación (AEI); Spiga, A. [0000-0002-6776-6268]; Murdoch, N. [0000-0002-9701-4075]; Lorenz, R. [0000-0001-8528-4644]; Forget, F. [0000-0002-3262-4366]; Newman, C. [0000-0001-9990-8817]; Rodríguez, S. [0000-0003-1219-0641]; Pla García, J. [0000-0002-8047-3937]; Viúdez Moreiras, D. [0000-0001-8442-3788]; Perrin, C. [0000-0002-7200-5682]; Mueller, N. T. [0000-0001-9229-8921]; Lemmon, M. [0000-0002-4504-5136]; Millour, E. [0000-0003-4808-9203]; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737
Studying the atmospheric planetary boundary layer (PBL) is crucial to understand the climate of a planet. The meteorological measurements by the instruments onboard InSight at a latitude of 4.5°N make a unique rich data set to study the active turbulent dynamics of the daytime PBL on Mars. Here we use the high-sensitivity continuous pressure, wind, and temperature measurements in the first 400 sols of InSight operations (from northern late winter to midsummer) to analyze wind gusts, convective cells, and vortices in Mars’ daytime PBL. We compare InSight measurements to turbulence-resolving large-eddy simulations (LES). The daytime PBL turbulence at the InSight landing site is very active, with clearly identified signatures of convective cells and a vast population of 6,000 recorded vortex encounters, adequately represented by a power law with a 3.4 exponent. While the daily variability of vortex encounters at InSight can be explained by the statistical nature of turbulence, the seasonal variability is positively correlated with ambient wind speed, which is supported by LES. However, wind gustiness is positively correlated to surface temperature rather than ambient wind speed and sensible heat flux, confirming the radiative control of the daytime Martian PBL; and fewer convective vortices are forming in LES when the background wind is doubled. Thus, the long-term seasonal variability of vortex encounters at the InSight landing site is mainly controlled by the advection of convective vortices by ambient wind speed. Typical tracks followed by vortices forming in the LES show a similar distribution in direction and length as orbital imagery.
Restringido
Constraints on the shallow elastic and anelastic structure of Mars from InSight seismic data
(Nature Research Journals, 2020-02-24) Lognonné, P.; Banerdt, W. B.; Pike, W. T.; Giardini, D.; Christensesn, U.; García, R. F.; Kawamura, T.; Kedar, S.; Knapmeyer Endrun, B.; Margerin, L.; Nimmo, F.; Panning, M.; Tauzin, B.; Scholz, J. R.; Antonangeli, D.; Barkaoui, S.; Beucler, E.; Bissig, F.; Brinkman, N.; Calvet, M.; Ceylan, S.; Charalambous, C.; Davis, P.; Van Driel, M.; Drilleau, M.; Fayon, L.; Joshi, R.; Kenda, B.; Khan, A.; Knapmeyer, M.; Lekic, V.; McClean, J.; Mimoun, D.; Murdoch, N.; Pan, L.; Perrin, C.; Pinot, B.; Pou, L.; Menina, S.; Rodríguez, Sébastien; Schmelzbach, C.; Schmerr, N.; Sollberg, D.; Spiga, A.; Stähler, S.; Stott, A.; Stutzmann, E.; Tharimena, S.; Widmer Schnidrig, R.; Andersson, F.; Ansan, V.; Beghein, C.; Knollenberg, M.; Krasner, S.; krause, C.; Lorenz, R.; Michaut, C.; Myhill, R.; Nissen Meyer, T.; Ten Pierick, J.; Plesa, A. C.; Quantin Nataf, C.; Robertsson, J.; Rochas, L.; Schimmel, M.; Smrekar, S.; Spohn, T.; Teanby, N.; Tromp, J.; Vallade, J.; Verdier, N.; Vrettos, C.; Weber, R.; Banfield, D.; Barrett, E.; Bierwith, M.; Calcutt, S.; Compaire, N.; Johnson, C. L.; Mance, D.; Euchner, F.; Kerjean, L.; Mainsant, G.; Mocquet, A.; Rodríguez Manfredi, J. A.; Pont, G.; Laudet, P.; Nebut, T.; Raucort, S.; Robert, O.; Russell, C. T.; Sylvestre Baron, A.; Tillier, S.; Warren, T.; Wieczorek, Mark A.; Yana, C.; Zweifel, P.; Centre National D'Etudes Spatiales (CNES); Agence Nationale de la Recherche (ANR); Lognonné, P.[0000-0002-1014-920X]; Spiga, A. [0000-0002-6776-6268]; Murdoch, N. [0000-0002-9701-4075]; Fayon, L. [0000-0002-4276-8160]; Knapmeyer, M. [0000-0003-0319-2514]; Tromp, J. [0000-0002-2742-8299]; Perrin, C. [0000-0002-7200-5682]; Schimmel, M. [0000-0003-2601-4462]; Panning, M. P. [0000-0002-2041-3190]; Rodríguez Manfredi, J. [0000-0003-0461-9815]; Pan, L. [0000-0002-8151-2125]; García, R. F. [0000-0003-1460-6663]; Rodríguez, S. [0000-0003-1219-0641]; Sollberger, D. [0000-0001-6408-6681]; Ceylan, S. [0000-0002-6552-6850]; Irving, J. [0000-0002-0866-8246]; Warren, T. [0000-0003-3877-0046]; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737
Mars’s seismic activity and noise have been monitored since January 2019 by the seismometer of the InSight (Interior Exploration using Seismic Investigations, Geodesy and Heat Transport) lander. At night, Mars is extremely quiet; seismic noise is about 500 times lower than Earth’s microseismic noise at periods between 4 s and 30 s. The recorded seismic noise increases during the day due to ground deformations induced by convective atmospheric vortices and ground-transferred wind-generated lander noise. Here we constrain properties of the crust beneath InSight, using signals from atmospheric vortices and from the hammering of InSight’s Heat Flow and Physical Properties (HP3) instrument, as well as the three largest Marsquakes detected as of September 2019. From receiver function analysis, we infer that the uppermost 8–11 km of the crust is highly altered and/or fractured. We measure the crustal diffusivity and intrinsic attenuation using multiscattering analysis and find that seismic attenuation is about three times larger than on the Moon, which suggests that the crust contains small amounts of volatiles.
Restringido
Initial results from the InSight mission on Mars
(Nature Research Journals, 2020-02-24) Banerdt, W. B.; Smrekar, S.; Banfield, D.; Giardini, D.; Golombek, M.; Johnson, C. L.; Lognonné, P.; Spiga, A.; Spohn, T.; Perrin, C.; Stähler, S.; Antonangeli, D.; Asmar, S.; Beghein, C.; Bowles, N.; Bozdag, E.; Chi, P.; Christensesn, U.; Clinton, J.; Collins, G. S.; Daubar, I.; Dehant, V.; Drilleau, M.; Fillingim, M.; Folkner, W.; García, R. F.; Garvin, J. B.; Grant, J.; Grott, M.; Grygorczuk, J.; Hudson, T.; Irving, J. C. E.; Kargl, G.; Kawamura, T.; Kedar, S.; King, S.; Knapmeyer Endrun, B.; Knapmeyer, M.; Lemmon, M. T.; Lorenz, R.; Maki, Justin N.; Margerin, L.; McLennan, S. M.; Michaut, C.; Mimoun, D.; Mittelholz, A.; Mocquet, A.; Morgan, P.; Mueller, N. T.; Murdoch, N.; Nagihara, S.; Newman, C. E.; Nimmo, F.; Panning, M.; Thomas Pike, W.; Plesa, A. C.; Rodríguez, Sébastien; Rodríguez Manfredi, J. A.; Russell, C. T.; Chmerr, N.; Siegler, M.; Stanley, S.; Stutzmann, E.; Teanby, N.; Tromp, J.; Van Driel, M.; Warner, N.; Weber, R.; Wieczorek, Mark A.; Agence Nationale de la Recherche (ANR); Swiss National Science Foundation (SNSF); Tromp, J. [0000-0002-2742-8299]; Rodríguez, S. [0000-0003-1219-0641]; Lognonné, P. [0000-0002-1014-920X]; Perrin, C. [0000-0002-7200-5682]; Murdoch, N. [0000-0002-9701-4075]; Knapmeyer, M. [0000-0003-0319-2514]; Rodríguez Manfredi, J. A. [0000-0003-0461-9815]; Spiga, A. [0000-0002-6776-6268]; Panning, M. P. [0000-0002-2041-3190]; García, R. [0000-0003-1460-6663]; Johnson, C. [0000-0001-6084-0149]; Stutzmann, E. [0000-0002-4348-7475]; Knapmeyer-Endrun, B. [0000-0003-3309-6785]; Schmerr, N. [0000-0002-3256-1262]; Irving, J. C. E. [0000-0002-0866-8246]; Morgan, P. [0000-0001-8714-4178]; Mueller, N. [0000-0001-9229-8921]; Pike, W. [0000-0002-7660-6231]; Kawamura, T. [0000-0001-5246-5561]; Clinton, J. [0000-0001-8626-2703]; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737
NASA’s InSight (Interior exploration using Seismic Investigations, Geodesy and Heat Transport) mission landed in Elysium Planitia on Mars on 26 November 2018. It aims to determine the interior structure, composition and thermal state of Mars, as well as constrain present-day seismicity and impact cratering rates. Such information is key to understanding the differentiation and subsequent thermal evolution of Mars, and thus the forces that shape the planet’s surface geology and volatile processes. Here we report an overview of the first ten months of geophysical observations by InSight. As of 30 September 2019, 174 seismic events have been recorded by the lander’s seismometer, including over 20 events of moment magnitude Mw = 3–4. The detections thus far are consistent with tectonic origins, with no impact-induced seismicity yet observed, and indicate a seismically active planet. An assessment of these detections suggests that the frequency of global seismic events below approximately Mw = 3 is similar to that of terrestrial intraplate seismic activity, but there are fewer larger quakes; no quakes exceeding Mw = 4 have been observed. The lander’s other instruments—two cameras, atmospheric pressure, temperature and wind sensors, a magnetometer and a radiometer—have yielded much more than the intended supporting data for seismometer noise characterization: magnetic field measurements indicate a local magnetic field that is ten-times stronger than orbital estimates and meteorological measurements reveal a more dynamic atmosphere than expected, hosting baroclinic and gravity waves and convective vortices. With the mission due to last for an entire Martian year or longer, these results will be built on by further measurements by the InSight lander.
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Joint Europa Mission (JEM): a multi-scale study of Europa to characterize its habitability and search for extant life
(Elsevier BV, 2020-11-15) Blanc, M.; Prieto Ballesteros, O.; André, N.; Gómez Elvira, J.; Jones, G.; Sterken, V.; Desprats, W.; Gurvits, L. I.; Khurana, K.; Balmino, G.; Blöcker, A.; Broquet, R.; Bunce, E.; Cavel, C.; Choblet, G.; Colins, G.; Coradini, M.; Cooper, J.; Dirkx, D.; Fontaine, D.; Garnier, P.; Gaudin, D.; Hartogh, P.; Hussmann, H.; Genova, A.; Less, L.; Jäggi, A.; Kempf, S.; Krupp, N.; Lara, L.; Lasue, J.; Lainey, V.; Leblanc, F.; Lebreton, J. P.; Longobardo, A.; Lorenz, R.; Martins, P.; Martins, Z.; Marty, J. C.; Masters, A.; Mimoun, D.; Palumba, E.; Parro García, V.; Regnier, P.; Saur, J.; Schutte, A.; Sittler, E. C.; Spohn, T.; Srama, R.; Stephan, K.; Szego, K.; Tosi, F.; Vance, S.; Wagner, R.; Van Hoolst, T.; Volwerk, M.; Wahlund, J. E.; Westall, F.; Wurz, P.; Ministerio de Economía y Competitividad (MINECO); Agencia Estatal de Investigación (AEI); 0000-0003-4002-2434; 0000-0002-2278-1210; 0000-0002-1797-2741; 0000-0002-9820-8584; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737
Europa is the closest and probably the most promising target to search for extant life in the Solar System, based on complementary evidence that it may fulfil the key criteria for habitability: the Galileo discovery of a sub-surface ocean; the many indications that the ice shell is active and may be partly permeable to transfer of chemical species, biomolecules and elementary forms of life; the identification of candidate thermal and chemical energy sources necessary to drive a metabolic activity near the ocean floor. In this article we are proposing that ESA collaborates with NASA to design and fly jointly an ambitious and exciting planetary mission, which we call the Joint Europa Mission (JEM), to reach two objectives: perform a full characterization of Europa's habitability with the capabilities of a Europa orbiter, and search for bio-signatures in the environment of Europa (surface, subsurface and exosphere) by the combination of an orbiter and a lander. JEM can build on the advanced understanding of this system which the missions preceding JEM will provide: Juno, JUICE and Europa Clipper, and on the Europa lander concept currently designed by NASA (Maize, report to OPAG, 2019). We propose the following overarching goals for our Joint Europa Mission (JEM): Understand Europa as a complex system responding to Jupiter system forcing, characterize the habitability of its potential biosphere, and search for life at its surface and in its sub-surface and exosphere. We address these goals by a combination of five Priority Scientific Objectives, each with focused measurement objectives providing detailed constraints on the science payloads and on the platforms used by the mission. The JEM observation strategy will combine three types of scientific measurement sequences: measurements on a high-latitude, low-altitude Europan orbit; in-situ measurements to be performed at the surface, using a soft lander; and measurements during the final descent to Europa's surface. The implementation of these three observation sequences will rest on the combination of two science platforms: a soft lander to perform all scientific measurements at the surface and sub-surface at a selected landing site, and an orbiter to perform the orbital survey and descent sequences. We describe a science payload for the lander and orbiter that will meet our science objectives. We propose an innovative distribution of roles for NASA and ESA; while NASA would provide an SLS launcher, the lander stack and most of the mission operations, ESA would provide the carrier-orbiter-relay platform and a stand-alone astrobiology module for the characterization of life at Europa's surface: the Astrobiology We Laboratory (AWL). Following this approach, JEM will be a major exciting joint venture to the outer Solar System of NASA and ESA, working together toward one of the most exciting scientific endeavours of the 21st century: to search for life beyond our own planet.
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The atmosphere of Mars as observed by InSight.
(Nature Research Journals, 2020-02-24) Banfield, D.; Spiga, A.; Newman, C. E.; Forget, F.; Lemmon, M. T.; Lorenz, R.; Murdoch, N.; Viúdez Moreiras, Daniel; Pla García, J.; García, R. F.; Lognonné, P.; Karatekin, Özgür; Perrin, C.; Martire, L.; Teanby, N.; Van Hove, B.; Maki, Justin N.; Kenda, B.; Mueller, N. T.; Rodriguez, Sébastien; Kawamura, T.; McClean, J. B.; Stott, A. E.; Charalambous, C.; Millour, E.; Johnson, C. L.; Mittelholz, A.; Määttänen, A.; Lewis, S. R.; Clinton, J.; Stähler, S. C.; Ceylan, S.; Giardini, D.; Warren, T.; Pike, W. T.; Daubar, I.; Golombek, M.; Rolland, L.; Widmer Schnidrig, R.; Mimoun, D.; Beucler, E.; Jacob, A.; Lucas, A.; Baker, M.; Ansan, V.; Hurst, K.; Mora Sotomayor, L.; Navarro, Sara; Torres, J.; Lepinette, A.; Molina, A.; Marín Jiménez, M.; Gómez Elvira, J.; Peinado, V.; Rodríguez Manfredi, J. A.; Carchic, B. T.; Sackett, S.; Russell, C. T.; Spohn, T.; Smrekar, S. E.; Banerdt, W. B.; Agence Nationale de la Recherche (ANR); Määttänen, A. [0000-0002-7326-8492]; Martire, L. [0000-0002-9402-6150]; Rodríguez Manfredi, J. A. [0000-0003-0461-9815]; Lognonné, P. [0000-0002-1014-920X]; Rodríguez, S. [0000-0003-1219-0641]; Spiga, A. [0000-0002-6776-6268]; Perrin, C. [0000-0002-7200-5682]; Molina, A. [0000-0002-5038-2022]; Rodríguez Manfredi, J. A. [0000-0003-0461-9815]; García, R. [0000-0003-1460-6663]; Murdoch, N. [0000-0002-9701-4075]; Lorenz, R. [0000-0001-8528-4644]; Mittelholz, A. [0000-0002-5603-7334]; Kawamura, T. [0000-0001-5246-5561]; Widmer Schnidrig, R. [0000-0001-9698-2739]; McClean, J. [0000-0002-7863-0120]; Mueller, N. [0000-0001-9229-8921]; Lewis, S. [0000-0001-7237-6494]; Teanby, N. [0000-0003-3108-5775]; Warren, T. [0000-0003-3877-0046]; Milliour, E. [0000-0003-4808-9203]; Lemmon, M. [0000-0002-4504-5136]; Clinton, J. [0000-0001-8626-2703]; Ceylan, S. [0000-0002-6552-6850]; Banfield, D. [0000-0003-2664-0164]; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737
The atmosphere of Mars is thin, although rich in dust aerosols, and covers a dry surface. As such, Mars provides an opportunity to expand our knowledge of atmospheres beyond that attainable from the atmosphere of the Earth. The InSight (Interior Exploration using Seismic Investigations, Geodesy and Heat Transport) lander is measuring Mars’s atmosphere with unprecedented continuity, accuracy and sampling frequency. Here we show that InSight unveils new atmospheric phenomena at Mars, especially in the higher-frequency range, and extends our understanding of Mars’s meteorology at all scales. InSight is uniquely sensitive to large-scale and regional weather and obtained detailed in situ coverage of a regional dust storm on Mars. Images have enabled high-altitude wind speeds to be measured and revealed airglow—faint emissions produced by photochemical reactions—in the middle atmosphere. InSight observations show a paradox of aeolian science on Mars: despite having the largest recorded Martian vortex activity and dust-devil tracks close to the lander, no visible dust devils have been seen. Meteorological measurements have produced a catalogue of atmospheric gravity waves, which included bores (soliton-like waves). From these measurements, we have discovered Martian infrasound and unexpected similarities between atmospheric turbulence on Earth and Mars. We suggest that the observations of Mars’s atmosphere by InSight will be key for prediction capabilities and future exploration.