High precision Mg isotope measurements of meteoritic samples by secondary ion mass spectrometry

Luu, Tu-Han; Chaussidon, M.; Mishra, R. K.; Rollion‐Bard, Claire; Villeneuve, Johan; Srinivasan, G.; Birck, J. L.

doi:10.1039/c2ja30187c

Cited by 21 publications

(15 citation statements)

References 40 publications

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“…Error bars represent uncertainties of the Δ 26 Mg Cpx-Grt value (i.e., ±0.07 × √ 2 ≈ ±0.10 ‰, 2SD). Data for Shuanghe and Hong'an eclogites are from Table 5, data for Bixiling eclogites are from Li et al (2011), and data for cratonic eclogites are from Wang et al (2012Wang et al ( , 2015a (Young et al 2002;Norman et al 2006;Pearson et al 2006;Xie et al 2011;Luu et al 2013;Sio et al 2013;Oeser et al 2015).…”

Section: Potential Applications In High-temperature Mg Isotope Geochementioning

confidence: 99%

Empirical calibration of the clinopyroxene–garnet magnesium isotope geothermometer and implications

Teng

Xiao

et al. 2016

Contrib Mineral Petrol

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between clinopyroxene and garnet. The equilibrium Δ 26 Mg clinopyroxene-garnet and corresponding temperature data obtained in this study, together with those available so far in literatures for natural eclogites, are used to calibrate the clinopyroxene-garnet Mg isotope thermometer. This yields a function of Δ 26 Mg clinopyroxene-garnet = (0.99 ± 0.06) × 10 6 /T 2 , where T is temperature in Kelvin. The refined function not only provides the best empirically calibrated clinopyroxene-garnet Mg isotope thermometer for precise constraints of temperatures of clinopyroxene-and garnet-bearing rocks, but also has potential applications in high-temperature Mg isotope geochemistry.

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Section: Potential Applications In High-temperature Mg Isotope Geochementioning

confidence: 99%

Empirical calibration of the clinopyroxene–garnet magnesium isotope geothermometer and implications

Teng

Xiao

et al. 2016

Contrib Mineral Petrol

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“…Major recent advances have been obtained from the development of high-precision measurements of the Mg isotopic compositions of CAIs and chondrules (6)(7)(8)(9)(10), increasing the resolution of 26 Al−…”

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confidence: 99%

Short time interval for condensation of high-temperature silicates in the solar accretion disk

Luu

Young

Gounelle

et al. 2015

Proc. Natl. Acad. Sci. U.S.A.

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Chondritic meteorites are made of primitive components that record the first steps of formation of solids in our Solar System. Chondrules are the major component of chondrites, yet little is known about their formation mechanisms and history within the solar protoplanetary disk (SPD . In addition, mineral 26 Al isochrons determined on the same chondrules show that their formation (i.e., fusion of their precursors by energetic events) took place from 0 Myr to ∼2 Myr after the formation of their precursors, thus showing in some cases a clear decoupling in time between the two events. The finding of a minimum bulk chondrule 26 Al isochron is used to constrain the astrophysical settings for chondrule formation. Either the temperature of the condensation zone dropped below the condensation temperature of chondrule precursors at ∼1.5 My after the start of the Solar System or the transport of precursors from the condensation zone to potential storage sites stopped after 1.5 My, possibly due to a drop in the disk accretion rate.Mg isotope analyses | MC-SIMS | HR-MC-ICPMS | chondrule history | short-lived 26 Al P rimitive meteorites (i.e., chondrites) are rocks that escaped melting and differentiation on their parent bodies. As a result, their components preserved a record of the mineralogy, chemistry, and isotopic compositions of the solids formed in the solar protoplanetary disk (SPD) before planetesimal formation. Viscous heating in the inner regions of the SPD (1) brought presolar dust and gas to temperatures higher than the sublimation point of most minerals, producing a gas that upon cooling produced the first Solar System solids by condensation. The relative uniformity of isotope ratios among many early Solar System materials (2) is testament to this phase of homogenization. The calcium−aluminum-rich inclusions (CAIs) that are found in primitive meteorites are considered to be formed from refractory precursors condensed at temperatures in the range from ∼1,400 K to ∼1,800 K (3). Chondrules are millimeter-size once-molten silicate spherules that comprise most of the mass (70-80%) of chondrites. They have compositions indicating that their formation took place from solid precursors condensed below 1,500 K (4, 5). The exact timing (duration, chronology) of (i) the condensation processes that produced the precursors of CAIs and of chondrules, and (ii) the processes that resulted in the formation of CAIs and chondrules, is still poorly known, although it is key to a better understanding of the complex origin and evolution of solids in the solar accretion disk.

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“…Measurements for which drastic changes of the background were observed were systematically discarded. Matrix effects on instrumental fractionation of Mg isotopes and on Al/Mg ion yields were determined through analyses of a suite of appropriate international (Burma spinel, San Carlos olivine, Vitim MORB) and in-house (melilite (Åk70), melilite2 (Åk20), Bacati) mineral and glass standards (Luu et al, 2013). After correction for matrix effects, the radiogenic excess ( 26 Mg*) was calculated by assuming an exponential law for Mg isotopic fractionation with a value of 0.514 for the exponent β (Davis and Richter, 2005).…”

Section: Ion Microprobe Analysismentioning

confidence: 99%

“…Mg isotope ratios and Al/Mg elemental ratios were determined in multicollection mode following the analytical protocol detailed by Luu et al (2013). Secondary 24 Mg + , 25 Mg + , 26 Mg + , and 27 Al + ions generated by a 13 kV oxygen primary beam of ~25 μm spot size and ~20-25 nA intensity were accelerated to 10 kV and analyzed using four Faraday cups (L'2, C, H1, H'2) at a mass resolving power (M/M) of ~2500 (exit slit #1 of the multicollector).…”

Section: Ion Microprobe Analysismentioning

confidence: 99%

“…However, the  26 Mg* i of the present CAI (-0.02 ± 0.23 ‰) has too large an uncertainty to exclude that the CAI exchanged its Mg isotopes with the nebular gas during the last melting event. The value of  26 Mg* i is governed by: Mg/ 24 Mg) DSM3 = 0.1398633 (i.e., the Mg isotope ratio of the international standard DSM3; e.g.,Luu et al, 2013). Assuming, for example, a bulk 27 Al/ 24 Mg ratio of 3 for the CAI, its  26 Mg* i would have reached a maximum of +0.11 ‰ in case of closed system evolution during 148 ka, as compared to -0.029 ‰ in case of total isotopic re-equilibration with the nebular gas ( 27 Al/ 24 Mg solar = 0.101;Lodders, 2003).…”

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confidence: 97%

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Evidence for an early nitrogen isotopic evolution in the solar nebula from volatile analyses of a CAI from the CV3 chondrite NWA 8616

Füri

Chaussidon

Marty

2015

Geochimica et Cosmochimica Acta

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High precision Mg isotope measurements of meteoritic samples by secondary ion mass spectrometry

Cited by 21 publications

References 40 publications

Empirical calibration of the clinopyroxene–garnet magnesium isotope geothermometer and implications

Empirical calibration of the clinopyroxene–garnet magnesium isotope geothermometer and implications

Short time interval for condensation of high-temperature silicates in the solar accretion disk

Evidence for an early nitrogen isotopic evolution in the solar nebula from volatile analyses of a CAI from the CV3 chondrite NWA 8616

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