FRINK Linked Data Fragments server

Matches in SemOpenAlex for { <https://semopenalex.org/work/W2105292824> ?p ?o ?g. }

• W2105292824 endingPage "230" @default.
• W2105292824 startingPage "197" @default.
• W2105292824 abstract "The early development of Mars is of enormous interest, not just in its own right, but also because it provides unique insights into the earliest history of the Earth, a planet whose origins have been all but obliterated. Mars is not as depleted in moderately volatile elements as are other terrestrial planets. Judging by the data for Martian meteorites it has Rb/Sr ≈ 0.07 and K/U ≈ 19,000, both of which are roughly twice as high as the values for the Earth. The mantle of Mars is also twice as rich in Fe as the mantle of the Earth, the Martian core being small (~20% by mass). This is thought to be because conditions were more oxidizing during core formation. For the same reason a number of elements that are moderately siderophile on Earth such as P, Mn, Cr and W, are more lithophile on Mars. The very different apparent behavior of high field strength (HFS) elements in Martian magmas compared to terrestrial basalts and eucrites may be related to this higher phosphorus content. The highly siderophile element abundance patterns have been interpreted as reflecting strong partitioning during core formation in a magma ocean environment with little if any late veneer. Oxygen isotope data provide evidence for the relative proportions of chondritic components that were accreted to form Mars. However, the amount of volatile element depletion predicted from these models does not match that observed — Mars would be expected to be more depleted in volatiles than the Earth. The easiest way to reconcile these data is for the Earth to have lost a fraction of its moderately volatile elements during late accretionary events, such as giant impacts. This might also explain the nonchondritic Si/Mg ratio of the silicate portion of the Earth. The lower density of Mars is consistent with this interpretation, as are isotopic data. 87Rb-87Sr, 129I-129Xe, 146Sm-142Nd, 182Hf-182W, 187Re-187Os, 235U-207Pb and 238U-206Pb isotopic data for Martian meteorites all provide evidence that Mars accreted rapidly and at an early stage differentiated into atmosphere, mantle and core. Variations in heavy xenon isotopes have proved complicated to interpret in terms of 244Pu decay and timing because of fractionation thought to be caused by hydrodynamic escape. There are, as yet, no resolvable isotopic heterogeneities identified in Martian meteorites resulting from 92Nb decay to 92Zr, consistent with the paucity of perovskite in the martian interior and its probable absence from any Martian magma ocean. Similarly the longer-lived 176Lu-176Hf system also preserves little record of early differentiation. In contrast W isotope data, Ba/W and time-integrated Re/Os ratios of Martian meteorites provide powerful evidence that the mantle retains remarkably early heterogeneities that are vestiges of core metal segregation processes that occurred within the first 20 Myr of the Solar System. Despite this evidence for rapid accretion and differentiation, there is no evidence that Mars grew more quickly than the Earth at an equivalent size. Mars appears to have just stopped growing earlier because it did not undergo late stage (>20 Myr) impacts on the scale of the Moon-forming Giant Impact that affected the Earth." @default.
• W2105292824 created "2016-06-24" @default.
• W2105292824 creator A5010262811 @default.
• W2105292824 creator A5055666059 @default.
• W2105292824 creator A5067413841 @default.
• W2105292824 creator A5079130781 @default.
• W2105292824 date "2001-01-01" @default.
• W2105292824 modified "2023-10-16" @default.
• W2105292824 title "The Accretion, Composition and Early Differentiation of Mars" @default.
• W2105292824 cites W1592004929 @default.
• W2105292824 cites W1600775227 @default.
• W2105292824 cites W1623958048 @default.
• W2105292824 cites W1660739765 @default.
• W2105292824 cites W1964072470 @default.
• W2105292824 cites W1964409922 @default.
• W2105292824 cites W1969628171 @default.
• W2105292824 cites W1970548478 @default.
• W2105292824 cites W1973257832 @default.
• W2105292824 cites W1973363072 @default.
• W2105292824 cites W1975440896 @default.
• W2105292824 cites W1976201010 @default.
• W2105292824 cites W1977082362 @default.
• W2105292824 cites W1979696967 @default.
• W2105292824 cites W1980076120 @default.
• W2105292824 cites W1980306400 @default.
• W2105292824 cites W1980705055 @default.
• W2105292824 cites W1981353386 @default.
• W2105292824 cites W1983389681 @default.
• W2105292824 cites W1986713906 @default.
• W2105292824 cites W1987907556 @default.
• W2105292824 cites W1991214217 @default.
• W2105292824 cites W1996990903 @default.
• W2105292824 cites W1998133890 @default.
• W2105292824 cites W2001030150 @default.
• W2105292824 cites W2003142147 @default.
• W2105292824 cites W2009585378 @default.
• W2105292824 cites W2012434233 @default.
• W2105292824 cites W2014465821 @default.
• W2105292824 cites W2015527356 @default.
• W2105292824 cites W2016611062 @default.
• W2105292824 cites W2017950907 @default.
• W2105292824 cites W2021648887 @default.
• W2105292824 cites W2022175403 @default.
• W2105292824 cites W2023564581 @default.
• W2105292824 cites W2027855284 @default.
• W2105292824 cites W2029364414 @default.
• W2105292824 cites W2032056660 @default.
• W2105292824 cites W2032839573 @default.
• W2105292824 cites W2033132055 @default.
• W2105292824 cites W2035635717 @default.
• W2105292824 cites W2036773053 @default.
• W2105292824 cites W2042212835 @default.
• W2105292824 cites W2043691935 @default.
• W2105292824 cites W2048506031 @default.
• W2105292824 cites W2048536106 @default.
• W2105292824 cites W2049711752 @default.
• W2105292824 cites W2054160977 @default.
• W2105292824 cites W2057485478 @default.
• W2105292824 cites W2058347696 @default.
• W2105292824 cites W2060637041 @default.
• W2105292824 cites W2061049947 @default.
• W2105292824 cites W2065123560 @default.
• W2105292824 cites W2065421390 @default.
• W2105292824 cites W2067432880 @default.
• W2105292824 cites W2068998009 @default.
• W2105292824 cites W2070884219 @default.
• W2105292824 cites W2072266099 @default.
• W2105292824 cites W2072810302 @default.
• W2105292824 cites W2074267811 @default.
• W2105292824 cites W2074601567 @default.
• W2105292824 cites W2076332174 @default.
• W2105292824 cites W2077956414 @default.
• W2105292824 cites W2078321309 @default.
• W2105292824 cites W2082103081 @default.
• W2105292824 cites W2085040468 @default.
• W2105292824 cites W2088677050 @default.
• W2105292824 cites W2090726489 @default.
• W2105292824 cites W2093295975 @default.
• W2105292824 cites W2099551296 @default.
• W2105292824 cites W2100758318 @default.
• W2105292824 cites W2102530828 @default.
• W2105292824 cites W2118650276 @default.
• W2105292824 cites W2139725372 @default.
• W2105292824 cites W2140242855 @default.
• W2105292824 cites W2143855186 @default.
• W2105292824 cites W2148830159 @default.
• W2105292824 cites W2149938984 @default.
• W2105292824 cites W2153597165 @default.
• W2105292824 cites W2901005329 @default.
• W2105292824 cites W4232459068 @default.
• W2105292824 doi "https://doi.org/10.1007/978-94-017-1035-0_7" @default.
• W2105292824 hasPublicationYear "2001" @default.
• W2105292824 type Work @default.
• W2105292824 sameAs 2105292824 @default.
• W2105292824 citedByCount "22" @default.
• W2105292824 countsByYear W21052928242012 @default.
• W2105292824 countsByYear W21052928242013 @default.
• W2105292824 countsByYear W21052928242016 @default.

• next