Isotopes: From Earth to the Solar System

Clayton, Robert N.

doi:10.1146/annurev.earth.35.092006.145059

Cited by 21 publications

(10 citation statements)

References 97 publications

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“…A CAI from a comet yielded no detectable trace of 26 Al (i.e., 26 Al/ 27 Al < 10 − 5 ; Matzel et al 2010), and further work should tell whether this is due to formation before 26 Al homogenization or formation/resetting after 26 Al decay. Finally, in a rather counterintuitive way, such rapid mixing processes may also explain the presence of large-scale isotopic heterogeneities in the accretion disk that are known to be present at planetary scales for either major (oxygen; Clayton 2007, Clayton et al 1973 or trace (molybdenum; Dauphas et al 2002b) elements. Indeed, such processes could reveal isotopic anomalies from a globally homogeneous medium by aerodynamically sorting the grains in size, if grains of a certain dimension were to carry the isotopic anomalies.…”

Section: The Astrophysical Context Of Solar System Formation and The mentioning

confidence: 99%

A Perspective from Extinct Radionuclides on a Young Stellar Object: The Sun and Its Accretion Disk

Dauphas

Chaussidon

2011

Annu. Rev. Earth Planet. Sci.

189

138

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■ Abstract Meteorites, which are remnants of solar system formation, provide a direct glimpse into the dynamics and evolution of a young stellar object (YSO), namely our Sun. Much of our knowledge about the astrophysical context of the birth of the Sun, the chronology of planetary growth from micrometer-sized dust to terrestrial planets, and the activity of the young Sun comes from the study of extinct radionuclides such as 26 Al (t 1/2 = 0.717 Myr). Here we review how the signatures of extinct radionuclides (short-lived isotopes that were present when the solar system formed and that have now decayed below detection level) in planetary materials influence the current paradigm of solar system formation. Particular attention is given to tying meteorite measurements to remote astronomical observations of YSOs and modeling efforts. Some extinct radionuclides were inherited from the long-term chemical evolution of the Galaxy, others were injected into the solar system by a nearby supernova, and some were produced by particle irradiation from the T-Tauri Sun. The chronology inferred from extinct radionuclides reveals that dust agglomeration to form centimeter-sized particles in the inner part of the disk was very rapid (<50 kyr), planetesimal formation started early and spanned several million years, planetary embryos (possibly like Mars) were formed in a few million years, and terrestrial planets (like Earth) completed their growths several tens of million years after the birth of the Sun.

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Section: The Astrophysical Context Of Solar System Formation and The mentioning

confidence: 99%

A Perspective from Extinct Radionuclides on a Young Stellar Object: The Sun and Its Accretion Disk

Dauphas

Chaussidon

2011

Annu. Rev. Earth Planet. Sci.

189

138

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“…chondrites | achondrites | isotope O xygen and sulfur are the only two elements in solar system silicates that process an isotopic abundance anomaly at the whole-meteorite level (1)(2)(3). Both elements belong to group VI and are the 3rd and 10th most abundant elements in the solar system (with S/O ratio of 2.1%) (4,5), respectively.…”

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confidence: 99%

Sulfur isotopic fractionation in vacuum UV photodissociation of hydrogen sulfide and its potential relevance to meteorite analysis

Chakraborty

Jackson

Ahmed

et al. 2013

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

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Select meteoritic classes possess mass-independent sulfur isotopic compositions in sulfide and organic phases. Photochemistry in the solar nebula has been attributed as a source of these anomalies. Hydrogen sulfide (H 2 S) is the most abundant gas-phase species in the solar nebula, and hence, photodissociation of H 2 S by solar vacuum UV (VUV) photons (especially by Lyman-α radiation) is a relevant process. Because of experimental difficulties associated with accessing VUV radiation, there is a paucity of data and a lack of theoretical basis to test the hypothesis of a photochemical origin of mass-independent sulfur. Here, we present multiisotopic measurements of elemental sulfur produced during the VUV photolysis of H 2 S. Mass-independent sulfur isotopic compositions are observed. The observed isotopic fractionation patterns are wavelengthdependent. VUV photodissociation of H 2 S takes place through several predissociative channels, and the measured mass-independent fractionation is most likely a manifestation of these processes. Meteorite sulfur data are discussed in light of the present experiments, and suggestions are made to guide future experiments and models.chondrites | achondrites | isotope

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“…Ballentine et al (1991); Ballentine and Burnard (2002); and Ozima and Podosek, (2002), state that 20 Ne in shallow reservoirs, is highly indicative of introduction into the shallow groundwater reservoir because the crustal production of 20 Ne is negligible to that of 20 Ne from the atmosphere. The reason for the high 20 Ne in the atmosphere is because the earth trapped it there during planetary accretion (Clayton, 2007). Craig and Lupton (1976) state that in samples taken from mantle sources (volcanic gases and mid-ocean ridge basalt-MORB), 20 Ne as well as nucleogenic 21 Ne, were enriched relative to 22 Ne.…”

Section: Neonmentioning

confidence: 99%

Isotopic Analyses of Helium From Wells Located in the Four Corners Area, southwestern, Us

Halford¹

2019

Geological Society of America Abstracts With Programs

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Helium, the lightest noble gas, is a valuable resource located on the Colorado Plateau southwestern US. Helium, a proven, useful noble gas, has many applications in modern technology for its chemical, physical, and thermodynamic properties. As of this writing, the price of crude helium is ~40% greater than CH 4 , rendering the economic grade for direct and secondary extraction at 0.3% helium. The helium systems in the Four Corners area (i.e., the study area) are characterized utilizing the geochemistry of noble gases, hydrocarbons, and nonhydrocarbons (compositional and isotopic), as well as geologic mapping. The geochemistry delineates sources of gases, migration pathways, and potential trapping/sealing mechanisms of the helium system, which is a slight deviation from the petroleum system. Economic helium (>0.3%) is primarily found in Paleozoic intervals structurally trapped on the Four Corners Platform, the edge of the Defiance Uplift, and the edge of the Holbrook Basin. Thirty-one gas samples, isotopically analyzed, are from actively producing Paleozoic formations within five fields: Tocito Dome, Dineh-Bi-Keyah, Ratherford, Pinta Dome, and Navajo Springs. Helium concentrations range from 0.01% to >6.0% and incorporates a spectrum of other gas values associated with relatively similar Paleozoic formations.

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Isotopes: From Earth to the Solar System

Cited by 21 publications

References 97 publications

A Perspective from Extinct Radionuclides on a Young Stellar Object: The Sun and Its Accretion Disk

A Perspective from Extinct Radionuclides on a Young Stellar Object: The Sun and Its Accretion Disk

Sulfur isotopic fractionation in vacuum UV photodissociation of hydrogen sulfide and its potential relevance to meteorite analysis

Isotopic Analyses of Helium From Wells Located in the Four Corners Area, southwestern, Us

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