Variations in K/Th on Mars

G. Jeffrey Taylor; J. D. Stopar; William V. Boynton; S. Karunatillake; John M. Keller; J. Brückner; H. Wänke; G. Dreibus; Kris E. Kerry; Robert C. Reedy; Larry G. Evans; Richard D. Starr; L. M.V. Martel; S. W. Squyres; O. Gasnault; S. Maurice; C. d'Uston; P. Englert; J. M. Dohm; V. R. Baker; D. Hamara; Daniel M. Janes; Ann L. Sprague; Kyeong J. Kim; D. M. Drake; S. M. McLennan; B. C. Hahn

doi:10.1029/2006JE002676

Variations in K/Th on Mars

G. Jeffrey Taylor, J. D. Stopar, William V. Boynton, S. Karunatillake, John M. Keller, J. Brückner, H. Wänke, G. Dreibus, Kris E. Kerry, Robert C. Reedy, Larry G. Evans, Richard D. Starr, L. M.V. Martel, S. W. Squyres, O. Gasnault, S. Maurice, C. d'Uston, P. Englert, J. M. Dohm, V. R. BakerD. Hamara, Daniel M. Janes, Ann L. Sprague, Kyeong J. Kim, D. M. Drake, S. M. McLennan, B. C. Hahn

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60 Scopus citations

Abstract

K/Th determined by the Mars Odyssey Gamma Ray Spectrometer varies by a factor of 3 on Mars (3000 to 9000), but over 95% of the surface area has K/Th between 4000 and 7000. K/Th is distinctly lower than average in some areas, including west of Olympus Mons in the Amazonis Planitia, the region around Memnonia Fossae, Chryse Planitia, southeastern Arabia Terra, Syrtis Major Planum, and northwest of Apollinaris Patera. On the other hand, K/Th is distinctly higher than average in other areas, including the central part of Valles Marineris and the surrounding highlands, and in the northern part of Hellas. The generally modest variation in K/Th may be explained by inherent variations in igneous rocks and by variations in the extent of aqueous alteration.

Original language	English (US)
Article number	E03S06
Journal	Journal of Geophysical Research: Planets
Volume	112
Issue number	3
DOIs	https://doi.org/10.1029/2006JE002676
State	Published - Mar 20 2007

ASJC Scopus subject areas

Geochemistry and Petrology
Geophysics
Earth and Planetary Sciences (miscellaneous)
Space and Planetary Science
Atmospheric Science
Astronomy and Astrophysics
Oceanography

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10.1029/2006JE002676

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Taylor, G. J., Stopar, J. D., Boynton, W. V., Karunatillake, S., Keller, J. M., Brückner, J., Wänke, H., Dreibus, G., Kerry, K. E., Reedy, R. C., Evans, L. G., Starr, R. D., Martel, L. M. V., Squyres, S. W., Gasnault, O., Maurice, S., d'Uston, C., Englert, P., Dohm, J. M., ... Hahn, B. C. (2007). Variations in K/Th on Mars. Journal of Geophysical Research: Planets, 112(3), [E03S06]. https://doi.org/10.1029/2006JE002676

Taylor, GJ, Stopar, JD, Boynton, WV, Karunatillake, S, Keller, JM, Brückner, J, Wänke, H, Dreibus, G, Kerry, KE, Reedy, RC, Evans, LG, Starr, RD, Martel, LMV, Squyres, SW, Gasnault, O, Maurice, S, d'Uston, C, Englert, P, Dohm, JM, Baker, VR, Hamara, D, Janes, DM, Sprague, AL, Kim, KJ, Drake, DM, McLennan, SM & Hahn, BC 2007, 'Variations in K/Th on Mars', Journal of Geophysical Research: Planets, vol. 112, no. 3, E03S06. https://doi.org/10.1029/2006JE002676

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title = "Variations in K/Th on Mars",

abstract = "K/Th determined by the Mars Odyssey Gamma Ray Spectrometer varies by a factor of 3 on Mars (3000 to 9000), but over 95% of the surface area has K/Th between 4000 and 7000. K/Th is distinctly lower than average in some areas, including west of Olympus Mons in the Amazonis Planitia, the region around Memnonia Fossae, Chryse Planitia, southeastern Arabia Terra, Syrtis Major Planum, and northwest of Apollinaris Patera. On the other hand, K/Th is distinctly higher than average in other areas, including the central part of Valles Marineris and the surrounding highlands, and in the northern part of Hellas. The generally modest variation in K/Th may be explained by inherent variations in igneous rocks and by variations in the extent of aqueous alteration.",

author = "Taylor, {G. Jeffrey} and Stopar, {J. D.} and Boynton, {William V.} and S. Karunatillake and Keller, {John M.} and J. Br{\"u}ckner and H. W{\"a}nke and G. Dreibus and Kerry, {Kris E.} and Reedy, {Robert C.} and Evans, {Larry G.} and Starr, {Richard D.} and Martel, {L. M.V.} and Squyres, {S. W.} and O. Gasnault and S. Maurice and C. d'Uston and P. Englert and Dohm, {J. M.} and Baker, {V. R.} and D. Hamara and Janes, {Daniel M.} and Sprague, {Ann L.} and Kim, {Kyeong J.} and Drake, {D. M.} and McLennan, {S. M.} and Hahn, {B. C.}",

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AU - Taylor, G. Jeffrey

AU - Stopar, J. D.

AU - Boynton, William V.

AU - Karunatillake, S.

AU - Keller, John M.

AU - Brückner, J.

AU - Wänke, H.

AU - Dreibus, G.

AU - Kerry, Kris E.

AU - Reedy, Robert C.

AU - Evans, Larry G.

AU - Starr, Richard D.

AU - Martel, L. M.V.

AU - Squyres, S. W.

AU - Gasnault, O.

AU - Maurice, S.

AU - d'Uston, C.

AU - Englert, P.

AU - Dohm, J. M.

AU - Baker, V. R.

AU - Hamara, D.

AU - Janes, Daniel M.

AU - Sprague, Ann L.

AU - Kim, Kyeong J.

AU - Drake, D. M.

AU - McLennan, S. M.

AU - Hahn, B. C.

PY - 2007/3/20

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N2 - K/Th determined by the Mars Odyssey Gamma Ray Spectrometer varies by a factor of 3 on Mars (3000 to 9000), but over 95% of the surface area has K/Th between 4000 and 7000. K/Th is distinctly lower than average in some areas, including west of Olympus Mons in the Amazonis Planitia, the region around Memnonia Fossae, Chryse Planitia, southeastern Arabia Terra, Syrtis Major Planum, and northwest of Apollinaris Patera. On the other hand, K/Th is distinctly higher than average in other areas, including the central part of Valles Marineris and the surrounding highlands, and in the northern part of Hellas. The generally modest variation in K/Th may be explained by inherent variations in igneous rocks and by variations in the extent of aqueous alteration.

AB - K/Th determined by the Mars Odyssey Gamma Ray Spectrometer varies by a factor of 3 on Mars (3000 to 9000), but over 95% of the surface area has K/Th between 4000 and 7000. K/Th is distinctly lower than average in some areas, including west of Olympus Mons in the Amazonis Planitia, the region around Memnonia Fossae, Chryse Planitia, southeastern Arabia Terra, Syrtis Major Planum, and northwest of Apollinaris Patera. On the other hand, K/Th is distinctly higher than average in other areas, including the central part of Valles Marineris and the surrounding highlands, and in the northern part of Hellas. The generally modest variation in K/Th may be explained by inherent variations in igneous rocks and by variations in the extent of aqueous alteration.

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Variations in K/Th on Mars

Abstract

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