TY - JOUR
T1 - Compositions of coarse and fine particles in martian soils at gale
T2 - A window into the production of soils
AU - Cousin, A.
AU - Meslin, P.Y.
AU - Wiens, R.C.
AU - Rapin, W.
AU - Mangold, N.
AU - Fabre, C.
AU - Gasnault, O.
AU - Forni, O.
AU - Tokar, R.
AU - Ollila, A.
AU - Schröder, S.
AU - Lasue, J.
AU - Maurice, S.
AU - Sautter, V.
AU - Newsom, H.
AU - Vaniman, D.
AU - Mouélic, S. Le
AU - Dyar, D.
AU - Berger, G.
AU - Blaney, D.
AU - Nachon, M.
AU - Dromart, G.
AU - Lanza, N.
AU - Clark, B.
AU - Clegg, S.
AU - Goertz, W.
AU - Berger, J
AU - Barraclough, B.
AU - Delapp, D.
AU - Martin-Torres, Javier
AU - MSL Science Team
N1 - Godkänd; 2015; Bibliografisk uppgift: Javier Martín-Torres ingår i the MSL Science Team. Special Issue: First Year of MSL; 20150331 (ninhul)
2019-05-14T09:59:14.979+02:00
PY - 2015/3/15
Y1 - 2015/3/15
N2 - The ChemCam instrument onboard the Curiosity rover provides for the first time an opportunity to study martian soils at a sub-millimeter resolution. In this work, we analyzed 24 soil targets probed by ChemCam during the first 250 sols on Mars. Using the depth profile capability of the ChemCam LIBS (Laser-Induced Breakdown Spectroscopy) technique, we found that 45% of the soils contained coarse grains (>500 μm). Three distinct clusters have been detected: Cluster 1 shows a low SiO2 content; Cluster 2 corresponds to coarse grains with a felsic composition, whereas Cluster 3 presents a typical basaltic composition. Coarse grains from Cluster 2 have been mostly observed exposed in the vicinity of the landing site, whereas coarse grains from Clusters 1 and 3 have been detected mostly buried, and were found all along the rover traverse. The possible origin of these coarse grains was investigated. Felsic (Cluster 2) coarse grains have the same origin as the felsic rocks encountered near the landing site, whereas the origin of the coarse grains from Clusters 1 and 3 seems to be more global. Fine-grained soils (particle size < laser beam diameter which is between 300 and 500 μm) show a homogeneous composition all along the traverse, different from the composition of the rocks encountered at Gale. Although they contain a certain amount of hydrated amorphous component depleted in SiO2, possibly present as a surface coating, their overall chemical homogeneity and their close-to-basaltic composition suggest limited, or isochemical alteration, and a limited interaction with liquid water. Fine particles and coarse grains from Cluster 1 have a similar composition, and the former could derive from weathering of the latter. Overall martian soils have a bulk composition between that of fine particles and coarse grains. This work shows that the ChemCam instrument provides a means to study the variability of soil composition at a scale not achievable by bulk chemical analyses.
AB - The ChemCam instrument onboard the Curiosity rover provides for the first time an opportunity to study martian soils at a sub-millimeter resolution. In this work, we analyzed 24 soil targets probed by ChemCam during the first 250 sols on Mars. Using the depth profile capability of the ChemCam LIBS (Laser-Induced Breakdown Spectroscopy) technique, we found that 45% of the soils contained coarse grains (>500 μm). Three distinct clusters have been detected: Cluster 1 shows a low SiO2 content; Cluster 2 corresponds to coarse grains with a felsic composition, whereas Cluster 3 presents a typical basaltic composition. Coarse grains from Cluster 2 have been mostly observed exposed in the vicinity of the landing site, whereas coarse grains from Clusters 1 and 3 have been detected mostly buried, and were found all along the rover traverse. The possible origin of these coarse grains was investigated. Felsic (Cluster 2) coarse grains have the same origin as the felsic rocks encountered near the landing site, whereas the origin of the coarse grains from Clusters 1 and 3 seems to be more global. Fine-grained soils (particle size < laser beam diameter which is between 300 and 500 μm) show a homogeneous composition all along the traverse, different from the composition of the rocks encountered at Gale. Although they contain a certain amount of hydrated amorphous component depleted in SiO2, possibly present as a surface coating, their overall chemical homogeneity and their close-to-basaltic composition suggest limited, or isochemical alteration, and a limited interaction with liquid water. Fine particles and coarse grains from Cluster 1 have a similar composition, and the former could derive from weathering of the latter. Overall martian soils have a bulk composition between that of fine particles and coarse grains. This work shows that the ChemCam instrument provides a means to study the variability of soil composition at a scale not achievable by bulk chemical analyses.
U2 - 10.1016/j.icarus.2014.04.052
DO - 10.1016/j.icarus.2014.04.052
M3 - Article
SN - 0019-1035
VL - 249
SP - 22
EP - 42
JO - Icarus (New York, N.Y. 1962)
JF - Icarus (New York, N.Y. 1962)
ER -