Morphology and composition of the surface of Mars: Mars Odyssey THEMIS results

Philip Christensen; Joshua L. Bandfield; James Bell; Noel Gorelick; Victoria E. Hamilton; Anton Ivanov; Bruce M. Jakosky; Hugh H. Kieffer; Melissa D. Lane; Michael C. Malin; Timothy McConnochie; Alfred S. McEwen; Harry Y. McSween; Greg L. Mehall; Jeffery E. Moersch; Kenneth H. Nealson; James W. Rice; Mark I. Richardson; Steven Ruff; Michael D. Smith; Timothy N. Titus; Michael B. Wyatt

doi:10.1126/science.1080885

Morphology and composition of the surface of Mars: Mars Odyssey THEMIS results

Philip Christensen, Joshua L. Bandfield, James Bell, Noel Gorelick, Victoria E. Hamilton, Anton Ivanov, Bruce M. Jakosky, Hugh H. Kieffer, Melissa D. Lane, Michael C. Malin, Timothy McConnochie, Alfred S. McEwen, Harry Y. McSween, Greg L. Mehall, Jeffery E. Moersch, Kenneth H. Nealson, James W. Rice, Mark I. Richardson, Steven Ruff, Michael D. SmithTimothy N. Titus, Michael B. Wyatt

Research output: Contribution to journal › Article › peer-review

307 Scopus citations

Abstract

The Thermal Emission Imaging System (THEMIS) on Mars Odyssey has produced infrared to visible wavelength images of the martian surface that show lithologically distinct layers with variable thickness, implying temporal changes in the processes or environments during or after their formation. Kilometer-scale exposures of bedrock are observed; elsewhere airfall dust completely mantles the surface over thousands of square kilometers. Mars has compositional variations at 100-meter scales, for example, an exposure of olivine-rich basalt in the walls of Ganges Chasma. Thermally distinct ejecta facies occur around some craters with variations associated with crater age. Polar observations have identified temporal patches of water frost in the north polar cap. No thermal signatures associated with endogenic heat sources have been identified.

Original language	English (US)
Pages (from-to)	2056-2061
Number of pages	6
Journal	Science
Volume	300
Issue number	5628
DOIs	https://doi.org/10.1126/science.1080885
State	Published - Jun 27 2003

ASJC Scopus subject areas

General

Access to Document

10.1126/science.1080885

Cite this

Christensen, P., Bandfield, J. L., Bell, J., Gorelick, N., Hamilton, V. E., Ivanov, A., Jakosky, B. M., Kieffer, H. H., Lane, M. D., Malin, M. C., McConnochie, T., McEwen, A. S., McSween, H. Y., Mehall, G. L., Moersch, J. E., Nealson, K. H., Rice, J. W., Richardson, M. I., Ruff, S., ... Wyatt, M. B. (2003). Morphology and composition of the surface of Mars: Mars Odyssey THEMIS results. Science, 300(5628), 2056-2061. https://doi.org/10.1126/science.1080885

Christensen, P, Bandfield, JL, Bell, J, Gorelick, N, Hamilton, VE, Ivanov, A, Jakosky, BM, Kieffer, HH, Lane, MD, Malin, MC, McConnochie, T, McEwen, AS, McSween, HY, Mehall, GL, Moersch, JE, Nealson, KH, Rice, JW, Richardson, MI, Ruff, S, Smith, MD, Titus, TN & Wyatt, MB 2003, 'Morphology and composition of the surface of Mars: Mars Odyssey THEMIS results', Science, vol. 300, no. 5628, pp. 2056-2061. https://doi.org/10.1126/science.1080885

@article{f0925de6d36b494199a334ede6b5b89b,

title = "Morphology and composition of the surface of Mars: Mars Odyssey THEMIS results",

abstract = "The Thermal Emission Imaging System (THEMIS) on Mars Odyssey has produced infrared to visible wavelength images of the martian surface that show lithologically distinct layers with variable thickness, implying temporal changes in the processes or environments during or after their formation. Kilometer-scale exposures of bedrock are observed; elsewhere airfall dust completely mantles the surface over thousands of square kilometers. Mars has compositional variations at 100-meter scales, for example, an exposure of olivine-rich basalt in the walls of Ganges Chasma. Thermally distinct ejecta facies occur around some craters with variations associated with crater age. Polar observations have identified temporal patches of water frost in the north polar cap. No thermal signatures associated with endogenic heat sources have been identified.",

author = "Philip Christensen and Bandfield, {Joshua L.} and James Bell and Noel Gorelick and Hamilton, {Victoria E.} and Anton Ivanov and Jakosky, {Bruce M.} and Kieffer, {Hugh H.} and Lane, {Melissa D.} and Malin, {Michael C.} and Timothy McConnochie and McEwen, {Alfred S.} and McSween, {Harry Y.} and Mehall, {Greg L.} and Moersch, {Jeffery E.} and Nealson, {Kenneth H.} and Rice, {James W.} and Richardson, {Mark I.} and Steven Ruff and Smith, {Michael D.} and Titus, {Timothy N.} and Wyatt, {Michael B.}",

year = "2003",

month = jun,

day = "27",

doi = "10.1126/science.1080885",

language = "English (US)",

volume = "300",

pages = "2056--2061",

journal = "Science",

issn = "0036-8075",

publisher = "American Association for the Advancement of Science",

number = "5628",

}

TY - JOUR

T1 - Morphology and composition of the surface of Mars

T2 - Mars Odyssey THEMIS results

AU - Christensen, Philip

AU - Bandfield, Joshua L.

AU - Bell, James

AU - Gorelick, Noel

AU - Hamilton, Victoria E.

AU - Ivanov, Anton

AU - Jakosky, Bruce M.

AU - Kieffer, Hugh H.

AU - Lane, Melissa D.

AU - Malin, Michael C.

AU - McConnochie, Timothy

AU - McEwen, Alfred S.

AU - McSween, Harry Y.

AU - Mehall, Greg L.

AU - Moersch, Jeffery E.

AU - Nealson, Kenneth H.

AU - Rice, James W.

AU - Richardson, Mark I.

AU - Ruff, Steven

AU - Smith, Michael D.

AU - Titus, Timothy N.

AU - Wyatt, Michael B.

PY - 2003/6/27

Y1 - 2003/6/27

N2 - The Thermal Emission Imaging System (THEMIS) on Mars Odyssey has produced infrared to visible wavelength images of the martian surface that show lithologically distinct layers with variable thickness, implying temporal changes in the processes or environments during or after their formation. Kilometer-scale exposures of bedrock are observed; elsewhere airfall dust completely mantles the surface over thousands of square kilometers. Mars has compositional variations at 100-meter scales, for example, an exposure of olivine-rich basalt in the walls of Ganges Chasma. Thermally distinct ejecta facies occur around some craters with variations associated with crater age. Polar observations have identified temporal patches of water frost in the north polar cap. No thermal signatures associated with endogenic heat sources have been identified.

AB - The Thermal Emission Imaging System (THEMIS) on Mars Odyssey has produced infrared to visible wavelength images of the martian surface that show lithologically distinct layers with variable thickness, implying temporal changes in the processes or environments during or after their formation. Kilometer-scale exposures of bedrock are observed; elsewhere airfall dust completely mantles the surface over thousands of square kilometers. Mars has compositional variations at 100-meter scales, for example, an exposure of olivine-rich basalt in the walls of Ganges Chasma. Thermally distinct ejecta facies occur around some craters with variations associated with crater age. Polar observations have identified temporal patches of water frost in the north polar cap. No thermal signatures associated with endogenic heat sources have been identified.

UR - http://www.scopus.com/inward/record.url?scp=12444268458&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=12444268458&partnerID=8YFLogxK

U2 - 10.1126/science.1080885

DO - 10.1126/science.1080885

M3 - Article

C2 - 12791998

AN - SCOPUS:12444268458

SN - 0036-8075

VL - 300

SP - 2056

EP - 2061

JO - Science

JF - Science

IS - 5628

ER -

Morphology and composition of the surface of Mars: Mars Odyssey THEMIS results

Abstract

ASJC Scopus subject areas

Access to Document

Other files and links

Fingerprint

Cite this