Please wait a minute...
img img
Adv. Search
Advances in Earth Science  2010, Vol. 25 Issue (7): 691-697    DOI: 10.11867/j.issn.1001-8166.2010.07.0691
Articles     
Progresses in OMEGA/Mars Express Detecting Minerals on Mars
Zhu Minqiang, Zhou Wanpeng, Hu Quanyi
Digital Land Key Laboratory of Jiangxi Province, East China Institute of Technology, Fuzhou 344000, China
Download:  PDF (24096KB) 
Export:  BibTeX | EndNote (RIS)      
Abstract  

The paper mainly introduces the features of OMEGA/Mars Express instrument and acquired data, the atmospheric correction methods, and  recent progresses of mineral detection. Empirical Transmission Functions (ETF) is the relative effective atmospheric correction method up to now. The OMEGA data have successfully revealed the diversity and complex of Mars surface minerals and composition. The hydrated phyllosilicates, a family of aqueous alteration products, such as nontronite, chlorite and montmorillonite, are detected by OMEGA. These minerals are mainly associated with Noachian outcrops, which are consistent with an early active hydrological system, sustaining the long-term contact of igneous minerals with liquid water. The hydrated sulfates, such as gypsum, kieserite and polyhydrated sulfates, are identified on light-toned layered terrains. The existence of these minerals means that there have evaporates deposits on Mars which are related to water processes. Anhydrous ferric oxides formed in a slow superficial weathering are distributed in lowland over the northern hemisphere, without liquid water playing a major role across the planet. OMEGA can identify pyroxene and olivine. It discriminates between the high-calcium pyroxenes and low-calcium pyroxenes. The high-calcium pyroxenes dominate in low-albedo volcanic regions of Hesperian age, dark sand and crater ejecta. The low-calcium pyroxenes occur as moderate to bright outcrops in older, Noachian terrains. OMEGA can also discriminate the H2O ice and CO2 ice in varied high-albedo polar icecap area. The H2O ice absorption features are major in the 1.08 m, 1.25 m, 1.51 m and 2.0m. The H2O ice absorption depth  increases with the ice grain size. The CO2 ice can be identified by 1.43  m, 2.0  m and 2.6m absorption features.

Key words:  Mars express      OMEGA      Atmosphere correction      Mineral identification     
Received:  17 September 2009      Published:  10 July 2010
P173  
Corresponding Authors:  Zhu Minqiang     E-mail:  mqzhu@ecit.edu.cn
Service
E-mail this article
Add to my bookshelf
Add to citation manager
E-mail Alert
RSS
Articles by authors

Cite this article: 

Zhu Minqiang, Zhou Wanpeng, Hu Quanyi. Progresses in OMEGA/Mars Express Detecting Minerals on Mars. Advances in Earth Science, 2010, 25(7): 691-697.

URL: 

http://www.adearth.ac.cn/EN/10.11867/j.issn.1001-8166.2010.07.0691     OR     http://www.adearth.ac.cn/EN/Y2010/V25/I7/691

[1] NASA. The Mars Exploration Program′s Science Theme[EB/OL]. http://mars.jpl.nasa.gov/science/, 2006.
[2] Bibring J P, Combes M, Langevin Y, et al. Results from the ISM experiment[J].Nature,1989, 341: 591-593
[3] Christensen P R, Bandfield J L, Hamilton V E,et al. Mars global surveyor thermal emission spectrometer experiment[J].Journal of Geophysical Research,2001, 106 (E10): 23 823-23 871.
[4] Bibring J P, Langevin Y, Gendrin A, et al. Mars surface diversity as revealed by the OMEGA/Mars express observations[J].Science,2005, 307: 1 576-1 630.
[5] NASA. Compact Reconnaissance Imaging Spectrometer for Mars (CRISM)[EB/OL].http://crism. jhuapl.edu/instrument/innoDesign.php, 2007.
[6] Mustard J F, Poulet F, Gendrin A, et al. Olivine and pyroxene diversity in the crust of mars[J].Science,2005, 307: 1 594-1 597.
[7] Combe J P, Sotin C, Mouélis S Le,et al. Methodology of hyperspectral reflectance data analysis for mineralogical mapping of planetary surface: Application to OMEGA/Mars Express images[C]//36th Lunar and Planetary Science Conference, 2005.
[8] Guan H, Xie H, Zhu M. Development of an alternative Martain atmospheric correction algorithm for OMEGA/Mars Express imagery[C]//Proceeding of 37th Lunar and Planetary Science Conference. Huston, 2006.
[9] Gendrin A, Mangold N, Arvidson R,et al. Sulfates in martian layered terrains: The OMEGA/Mars express view[J].Science,2005, 307: 1 587-1 591.
[10] Langevin Y, Poulet F, Bibring J P, et al. Sulfates in the north Polar region of mars detected by OMEGA/Mars express[J].Science,2005, 307: 1 584-1 586.
[11] Poulet F, Bibring J P, Mustard J F, et al. Phyllosilicates on Mars and implications for early martian climate[J].Nature,2005, 438: 632-627.
[12] Bibring J P, Loizeau D, Pelkey S M, et al. Coupled OMEGA-CRISM observations of marwth vallis[C]//Proceedings of 38th Lunar and Planetary Science Conference. Huston, 2007.
[13] Bibring J P, Langevin Y, Mustard J F, et al. Global mineralogical and aqueous Mars history derived from OMEGA/Mars express data[J].Science,2006, 312: 400-404.
[14] Hale A S, Bass D S, Tamppari L K. Monitoring the perennial martian northern polar cap with MGS MOC[J].ICARUS,2005, 174: 502-512.
[15] Langevin Y, Poulet F, Bibring J P, et al. Summer evolution of the north polar cap of mars as observed by OMEGA/ Mars Express[J].Science,2005, 307: 1 581-1 584.
[16] Langevin Y, Doute S, Vincendon M, et al. No signature of clear CO2 ice from the cryptic′ regions in Mars′ south seasonal polar cap[J].Nature,2006,442: 790-792.
[17] Souza J P, Squyres S, Arvidson R, et al. Mars Mineralogy: Preliminary Results from Mars exploration Rovers Spirit and Opportunity[C]//Pecchio, Andrade, D′Agostino, et al, eds. Applied Mineralogy. São Paulo: ICAM BR, 2004.
[18] Bell J F, Squyres S, Arvidson R E, et al. Pancam multispectral imaging results from the opportunity rover at meridiani Planum[J].Science,2004, 306: 1 703-1 709.
[19] Christensen P R, Wyatt M B, Glotch T D, et al. Mineralogy at Meridiani Planum from the Mini-TES Experiment on the Opportunity Rover[J].Science,2004, 306: 1 733-1 739.
[20] Squyres S, Arvidson R E, Bell J F, et al. The opportunity rover′s athena science investigation at Meridiani Planum, Mars[J].Science,2004, 306: 1 698-1 703.
[21] Hynek B M, Arvidson R E, Phillips R J, et al. Geologic setting and origin of Terra Meridiani hematite deposit on Mars[J].Journal of Geophysical Research,2002, 107(E10):18-1-18-14.
[22] Zhu M, Guan H, Xie H. Mineral and Lithologic Mapping of Martian Low Albedo Regions Using OMEGA Data[C]//Proceedings of 37th Lunar and Planetary Science Conference. Huston, 2006.
[23] Arvidson R E, Seelos F P, Deal K,et al. Mantled and exhumed terrains in Terra Meridiani, Mars[J].Journal of Geophysical Research,2003, 108 (E12): 14-1-14-20.

No Suggested Reading articles found!