The Martian Meteorite Compendium
Oxygen Isotopes
Figure 1: Graph of oxygen isotopic composition of Martian Meteorites and mineral separates from data given in attached table (references therein). Data obtained over a number of years, by different techniques, in different laboratories, is not often in agreement, but differes significantly from that of other meteorites and from terrestrial samples. Data define a Mars mass fractionation line, offset from the terrestrial mass fractionation line by about +0.32 per mil (Franchi et al. 1999). Oxygen isotopic data is "per mil", relative to SMOW.
Oxygen isotopes are reported as delta = [(RSAM–RSTD)/RSTD] x 1000, where R =17O/16O and 18O/16O delta 17 and delta 18 and SAM and STD denote sample and standard. On a delta 17 and delta 18 plot, mass fractionation produces a nearly linear array with slope of 0.52. (see discussion in introduction)
Oxygen Isotopes - Martian Meteorites
delta 17 | delta 18 | DELTA 17 | reference | |
---|---|---|---|---|
Nakhla px | 2.69 | 4.55 | 0.32 | Clayton and Mayeda 1996 |
Nakhla ol | 2.49 | 4.1 | 0.36 | Clayton and Mayeda 1996 |
Nakhla | 3.017 | 5.216 | 0.305 | Franchi et al. 1999 |
Lafayette | 2.79 | 4.73 | 0.33 | Clayton and Mayeda 1996 |
Lafayette px. | 2.57 | 4.57 | 0.19 | Clayton and Mayeda 1996 |
Lafayette px. | 2.81 | 4.97 | 0.23 | Romanek et al. 1998 |
Lafayette ol. | 2.4 | 4.03 | 0.28 | Clayton and Mayeda 1996 |
Lafayette ol. | 2.56 | 4.35 | 0.31 | Romanek et al. 1998 |
Lafayette | 2.846 | 4.876 | 0.31 | Franchi et al. 1999 |
Lafayette | 2.99 | 5.17 | 0.3 | Romanek et al. 1998 |
Chassigny | 2.33 | 3.91 | 0.3 | Clayton and Mayeda 1996 |
Chassigny | 2.486 | 4.205 | 0.3 | Franchi et al. 1999 |
Chassigny | 2.64 | 4.46 | 0.32 | Romanek et al. 1998 |
Shergotty | 2.76 | 4.61 | 0.36 | Clayton and Mayeda 1996 |
Shergotty | 2.865 | 4.866 | 0.335 | Franchi et al. 1999 |
Shergotty | 2.97 | 5.06 | 0.34 | Romanek et al. 1998 |
Zagami | 2.75 | 4.55 | 0.38 | Clayton and Mayeda 1996 |
Zagami | 2.991 | 5.092 | 0.343 | Franchi et al. 1999 |
Zagami | 2.67 | 4.61 | 0.28 | Romanek et al. 1998 |
ALH77005 | 2.18 | 3.88 | 0.16 | Clayton and Mayeda 1996 |
ALH77005 | 2.64 | 4.449 | 0.326 | Franchi et al. 1999 |
EETA79001A | 2.46 | 4.23 | 0.28 | Clayton and Mayeda 1996 |
EETA79001A | 2.75 | 4.67 | 0.32 | Romanek et al. 1998 |
EETA79001B | 2.56 | 4.34 | 0.3 | Clayton and Mayeda 1996 |
EETA79001B | 2.67 | 4.64 | 0.25 | Romanek et al. 1998 |
EETA79001 | 2.6 | 4.382 | 0.321 | Franchi et al. 1999 |
LEW88516 | 2.39 | 4.14 | 0.26 | Clayton and Mayeda 1996 |
ALH84001 | 2.58 | 4.53 | 0.22 | Clayton and Mayeda 1996 |
ALH84001 | 2.743 | 4.644 | 0.327 | Franchi et al. 1999 |
QUE94201 | 2.8 | 4.97 | 0.19 | misprint C and M |
QUE94201 | 2.546 | 4.266 | 0.327 | Franchi et al. 1999 |
Y793605 | 2.3 | 4.01 | 0.21 | Clayton and Mayeda 1996 |
DaG476 | 2.692 | 4.567 | 0.317 | Franchi et al. 1999 |
DaG489 | 2.89 | 4.98 | 0.305 | Folco et al. 2000 |
DaG670 | 2.86 | 4.95 | 0.28 | Folco et al. 2000 |
Los Angeles | 2.53 | 4.53 | 0.17 | Rubin et al. 2000 |
SaU094 | 2.51 | 4.28 | 0.3 | Gnos et al. 2002 |
Dhofar019 | 2.99 | 5.4 | 0.18 | Taylor et al. 2002 |
NWA480 | 2.91 | 4.78 | 0.42 | Barett et al. 2002 |
NWA817 | 3.2 | 5.44 | 0.37 | Sautter et al. 2002 |
NWA856 | 3.09 | 5.03 | 0.47 | Jambon et al. 2001 |
Dhofar378 | 2.52 | 4.46 | Ikeda et al. 2002 | |
NWA998 | 2.2 | 3.9 | 0.24 | Irving et al. 2002 |
Y980459 | 2.52 | 4.31 | 0.28 | Japanese Newsletter |
YA1075 | 2.23 | 3.95 | 0.18 | Yanai 2002 |