TY - JOUR
T1 - Oxygen isotopes in crystalline silicates of comet Wild 2
T2 - A comparison of oxygen isotope systematics between wild 2 particles and chondritic materials
AU - Nakashima, Daisuke
AU - Ushikubo, Takayuki
AU - Joswiak, David J.
AU - Brownlee, Donald E.
AU - Matrajt, Graciela
AU - Weisberg, Michael K.
AU - Zolensky, Michael E.
AU - Kita, Noriko T.
N1 - Funding Information:
The manuscript was greatly improved by reviews from J. Aléon and an anonymous reviewer. The authors thank R.K. Noll for help with FIB and FE-SEM observation, H. Xu and P.E. Brown for use of a polarizing microscope and high magnification objective lens, J. Kern for SIMS support, and T.J. Tenner for kindly providing oxygen isotope data of CR3 chondrite chondrules and for discussion. R.C. Ogliore and K. Nagashima kindly provided us oxygen isotope data of the Wild 2 particle Iris for our discussion. This work is supported by various NASA programs ( NK, NNX09AC30G ; DB , NNX10AI89GS01 ; Cosmochemistry and Laboratory Analysis of Returned Samples Program to MZ). WiscSIMS is partly supported by NSF-EAR ( 0319230 , 0744079 , 1053466 ).
PY - 2012/12/1
Y1 - 2012/12/1
N2 - Oxygen three-isotope ratios of nine crystalline silicate particles from comet Wild 2 were measured to investigate oxygen isotope systematics of cometary materials. We are able to analyze particles as small as 4μm using an ion microprobe with a~1×2μm beam by locating the analysis spots with an accuracy of ±0.4μm. Three particles of Mn-rich forsterite, known as low-iron, manganese-enriched (LIME) olivine, showed extremely 16O-rich signatures (δ18O, δ17O~-50‰), similar to refractory inclusions in chondrites. The three Mn-rich forsterite particles may have formed by condensation from an 16O-rich solar nebula gas. Other particles consist of olivine and/or pyroxene with a wide range of Mg# [=molar MgO/(FeO+MgO) %] from 60 to 96. Their oxygen isotope ratios plot nearly along the carbonaceous chondrite anhydrous mineral (CCAM) and Young and Russell lines with Δ17O(=δ17O-0.52×δ18O) values of -3.0‰ to +2.5‰. These data are similar to the range observed from previous analyses of Wild 2 crystalline silicates and those of chondrules in carbonaceous chondrites. Six particles extracted from Stardust track 77 show diverse chemical compositions and isotope ratios; two Mn-rich forsterites, FeO-poor pigeonite, and three FeO-rich olivines with a wide range of Δ17O values from -24‰ to +1.6‰. These results confirmed that the original projectile that formed track 77 was an aggregate (>6μm) of silicate particles that formed in various environments.The Δ17O values of ferromagnesian Wild 2 particles (including data from previous studies) increase from ~-23‰ to+2.5‰ with decreasing Mg#: Δ17O values of Mn-rich forsterite particles (Mg#=98-99.8) cluster at -23‰, those of FeO-poor particles (Mg#=95-97) cluster at -2‰, and those of FeO-rich particles (Mg#≤90) scatter mainly from -1.5‰ to+2.5‰. Compared to chondrules in primitive chondrites, the systematic trend between Mg# and Δ17O among the Wild 2 particles is most similar to that reported for CR chondrite chondrules. We argue that CR chondrites and some cometary materials share multiple common chemical and isotope characteristics. We suggest that many of the crystalline silicate particles formed in the outer regions of the asteroid belt, or regions that share the common properties, and were transported to comet-forming regions and accreted into comet Wild 2.
AB - Oxygen three-isotope ratios of nine crystalline silicate particles from comet Wild 2 were measured to investigate oxygen isotope systematics of cometary materials. We are able to analyze particles as small as 4μm using an ion microprobe with a~1×2μm beam by locating the analysis spots with an accuracy of ±0.4μm. Three particles of Mn-rich forsterite, known as low-iron, manganese-enriched (LIME) olivine, showed extremely 16O-rich signatures (δ18O, δ17O~-50‰), similar to refractory inclusions in chondrites. The three Mn-rich forsterite particles may have formed by condensation from an 16O-rich solar nebula gas. Other particles consist of olivine and/or pyroxene with a wide range of Mg# [=molar MgO/(FeO+MgO) %] from 60 to 96. Their oxygen isotope ratios plot nearly along the carbonaceous chondrite anhydrous mineral (CCAM) and Young and Russell lines with Δ17O(=δ17O-0.52×δ18O) values of -3.0‰ to +2.5‰. These data are similar to the range observed from previous analyses of Wild 2 crystalline silicates and those of chondrules in carbonaceous chondrites. Six particles extracted from Stardust track 77 show diverse chemical compositions and isotope ratios; two Mn-rich forsterites, FeO-poor pigeonite, and three FeO-rich olivines with a wide range of Δ17O values from -24‰ to +1.6‰. These results confirmed that the original projectile that formed track 77 was an aggregate (>6μm) of silicate particles that formed in various environments.The Δ17O values of ferromagnesian Wild 2 particles (including data from previous studies) increase from ~-23‰ to+2.5‰ with decreasing Mg#: Δ17O values of Mn-rich forsterite particles (Mg#=98-99.8) cluster at -23‰, those of FeO-poor particles (Mg#=95-97) cluster at -2‰, and those of FeO-rich particles (Mg#≤90) scatter mainly from -1.5‰ to+2.5‰. Compared to chondrules in primitive chondrites, the systematic trend between Mg# and Δ17O among the Wild 2 particles is most similar to that reported for CR chondrite chondrules. We argue that CR chondrites and some cometary materials share multiple common chemical and isotope characteristics. We suggest that many of the crystalline silicate particles formed in the outer regions of the asteroid belt, or regions that share the common properties, and were transported to comet-forming regions and accreted into comet Wild 2.
KW - Comet 81P/Wild 2
KW - Crystalline silicate
KW - Oxygen isotope ratios
KW - Solar system formation
KW - Stardust
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U2 - 10.1016/j.epsl.2012.09.041
DO - 10.1016/j.epsl.2012.09.041
M3 - Article
AN - SCOPUS:84867808275
SN - 0012-821X
VL - 357-358
SP - 355
EP - 365
JO - Earth and Planetary Sciences Letters
JF - Earth and Planetary Sciences Letters
ER -