Physics
Scientific paper
Dec 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufm.p51a0901s&link_type=abstract
American Geophysical Union, Fall Meeting 2005, abstract #P51A-0901
Physics
1009 Geochemical Modeling (3610, 8410), 1027 Composition Of The Planets, 1060 Planetary Geochemistry (5405, 5410, 5704, 5709, 6005, 6008), 6225 Mars, 8450 Planetary Volcanism (5480, 6063, 8148)
Scientific paper
The shergottite, nakhlite and chassignite (SNC) meteorites are widely accepted as being of martian origin, and have been studied extensively in relation to chemical evolution of Mars. One of notable result of these studies is finding of 142Nd and 182W isotopic anomalies in SNC meteorites. As these isotopic anomalies should result from decay of the extinct radionuclides 146Sm and 182Hf, it is commonly interpreted that Mars accreted and differentiated rapidly (e.g., Lee and Halliday, 1997). Since this early differentiation process should accompany global magma ocean (Gaetani and Grove, 1997; Righter and Drake, 1996, 1997), it is plausible that the early differentiation process produced chemically stratified mantle (Borg et al. 2003; Shimoda et al., 2005). The magma source materials of the SNC meteorites (magmas) are considered to be products of the early differentiation process of Mars that are characterized by time-integrated LREE depletions or enrichments. As the degree of depletion is significantly greater than terrestrial magmas, it is suggested that Mars has chemically distinct reservoirs. Similar result is obtained by studies of Lu-W-Hf, Re-Os and 146Sm-142Nd systematics that indicate the presence of enriched and depleted reservoirs in Mar (Blichert-Toft et al., 1999; Brandon et al, 2000). These lines of isotopic evidence suggest that Mars preserves layered mantle structure that was produced during the early differentiation process. Although the martian geochemical reservoirs is commonly accepted, little constraint has been given to the chemical composition of the martian geochemical reservoirs. Recently, Shimoda et al (2005) have proposed a model to explain the origin of martian magmatism; the martian magmatism was induced by plume melting from the hydrated deepest mantle reservoir with depleted geochemical signature. Although the model successfully explains the chemical composition of SNC meteorites that have depleted geochemical characters, additional enriched geochemical reservoir is required to explain the chemical variation of SNC magmas. In the present study, we will discuss the isotopic and trace element composition of martian enriched reservoir.
Ikeda Yasufumi
Shimoda Gen
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