The NetLander geophysical network on the surface of Mars: General mission description and technical design status

Marsal, O.; Venet, M.; Counil, J. L.; Ferri, F.; Harri, A. M.; Spohn, Tilman; Block, Joern

doi:10.1016/s0094-5765(02)00069-3

Cited by 14 publications

(5 citation statements)

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“…Additionally, the inferred crustal thickness estimates indicate the thinner and thicker regions of the crust that may concentrate predominantly compressive and tensile stresses, respectively [ Artyushkov , 1973; von Frese et al , 1997a; Potts , 2000; Potts et al , 2002]. Hence the free‐air anomalies of visible and buried basins can be important for evaluating the residual stress field in the crust for not only the distribution of crustal fluids, but also crustal seismicity for passive seismic experiments, and other neotectonic crustal features that may help focus the selection of sites for geophysical subsurface imaging experiments [e.g., Marsal et al , 2002].…”

Section: Discussionmentioning

confidence: 99%

Gravity‐inferred crustal attributes of visible and buried impact basins on Mars

et al. 2004

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[1] The impact basins of Mars reveal important insights on Martian tectonic evolution. They involve strongly disrupted, depressed regions of crust with likely enhanced porosity and permeability that may locally concentrate water and other crustal fluids. Hence the crustal properties of impact basins can also be important in the hunt for water and related clues for life on Mars. We assess the crustal details of impact basins by separating the Mars Global Surveyor free-air anomalies into terrain-correlated and terrain-decorrelated components. The separation is based on the correlation spectrum between the free-air anomalies and the gravity effects evaluated from the topography mapped by the Mars Orbital Laser Altimeter (MOLA). For topographically visible multiring basins like Isidis, striking circular patterns of alternating terrain-correlated free-air maxima and minima mark the uncompensated components of the central mantle plug and surrounding rings. The first vertical derivatives of these anomalies effectively estimate the basin ring locations and a transient cavity depth-to-diameter ratio of 0.09 that is consistent with the ratio observed for lunar nearside multiring basins. For the Isidis Basin we obtain an excavation depth of roughly 66 km that reflects considerably disrupted crust for concentrating local fluids since the Noachian impact. Furthermore, the related crustal terrain-decorrelated free-air anomalies suggest up to 2 km of high-density basin fill may cap the central basin. Subtle quasi-circular depressions in the relatively featureless MOLA terrain of the northern hemisphere have identified potentially buried impact basins [Frey et al., 2002]. An altimetry depression in Acidalia Planitia and another in Utopia are also associated with ringed patterns of terrain-decorrelated free-air anomalies that may mark the uncompensated mass effects of buried impact basins. The gravity-derived transient excavation depths for these inferred basins are roughly 41 and 20 km, respectively, while the related ring diameters (D) follow the ubiquitous ffiffi ffi 2 p D rule of planetary impact basins. The crust of these buried basins is likely to contain water at higher levels than the crust of the equatorial basins that was substantially dewatered with the development of the great northern basin. Hence analyzing surface fractures, faults, and other crustal discontinuities that can tap the more saturated crust of these inferred buried basins may facilitate the hunt for water on Mars.

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Section: Discussionmentioning

confidence: 99%

Gravity‐inferred crustal attributes of visible and buried impact basins on Mars

et al. 2004

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“…More than 2 decades of efforts will have therefore been spent in proposal formulations and instrument development between the collapse of Mars 96 and the selection of InSight. See the summary provided by Lognonné (2005), including efforts related the NetLander project, a network of 4 landers cancelled at the end of its phase B (Harri et al 1999; Sotin et al 2000; Lognonné et al 2000; Banerdt and Pike 2001; Marsal et al 2002; Dehant et al 2004). We will describe only those directly related to the conception of InSight and SEIS.…”

Section: Mars Seismology Backgroundmentioning

confidence: 99%

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

et al. 2019

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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 ( S eismic E xperiment for I nternal S tructure) 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 at 1 Hz and 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 at 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. Electronic Supplementary Material The online version of this article (10.1007/s11214-018-0574-6) contains supplementary material, which is available to authorized users.

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“…The enthusiasm for this endeavor has been manifested in a number of mission studies including Mars Environmental Survey (MESUR) (Solomon et al, 1991;Hubbard et al, 1993;Squyres, 1995), MarsNet (Chicarro et al, 1991;1993), and InterMarsnet (Chicarro et al, 1994;Banerdt et al, 1996). At the beginning of the 21st century the goal was close to being realized with the NetLander mission (Lognonné et al, 1998;Harri et al, 1999;Counil et al, 2001;Marsal et al, 2002;Dehant et al, 2004), which was sponsored by a broad consortium of nations in Europe and America. Unfortunately, budget difficulties and programmatic conflicts at CNES and NASA resulted in its cancellation.…”

Section: What Kind Of Instruments Can Help Geophysical Studies?mentioning

confidence: 99%