Showing papers by "Gary R. Huss published in 2005"
24 Oct 2005
TL;DR: In this paper, the high-resolution Pb-Pb ages and short-lived nuclide based relative ages for CAIs and chondrules are reviewed. And the solar system started at 4567.2 {+-} 0.6Ma inferred from the high precision Pb Pb ages of CAIs.
Abstract: The high time resolution Pb-Pb ages and short-lived nuclide based relative ages for CAIs and chondrules are reviewed. The solar system started at 4567.2 {+-} 0.6Ma inferred from the high precision Pb-Pb ages of CAIs. Time scales of CAIs ({le}0.1Myr), chondrules (1-3Myr), and early asteroidal differentiation ({ge}3Myr) inferred from {sup 26}Al relative ages are comparable to the time scale estimated from astronomical observations of young star; proto star, classical T Tauri star and week-lined T Tauri star, respectively. Pb-Pb ages of chondrules also indicate chondrule formation occur within 1-3 Myr after CAIs. Mn-Cr isochron ages of chondrules are similar to or within 2 Myr after CAI formation. Chondrules from different classes of chondrites show the same range of {sup 26}Al ages in spite of their different oxygen isotopes, indicating that chondrule formed in the localized environment. The {sup 26}Al ages of chondrules in each chondrite class show a hint of correlation with their chemical compositions, which implies the process of elemental fractionation during chondrule formation events.
115 citations
24 Oct 2005
TL;DR: In this paper, the high-resolution Pb-Pb ages and short-lived nuclide based relative ages for CAIs and chondrules are reviewed. And the solar system started at 4567.2 {+-} 0.6Ma inferred from the high precision Pb Pb ages of CAIs.
Abstract: The high time resolution Pb-Pb ages and short-lived nuclide based relative ages for CAIs and chondrules are reviewed. The solar system started at 4567.2 {+-} 0.6Ma inferred from the high precision Pb-Pb ages of CAIs. Time scales of CAIs ({le}0.1Myr), chondrules (1-3Myr), and early asteroidal differentiation ({ge}3Myr) inferred from {sup 26}Al relative ages are comparable to the time scale estimated from astronomical observations of young star; proto star, classical T Tauri star and week-lined T Tauri star, respectively. Pb-Pb ages of chondrules also indicate chondrule formation occur within 1-3 Myr after CAIs. Mn-Cr isochron ages of chondrules are similar to or within 2 Myr after CAI formation. Chondrules from different classes of chondrites show the same range of {sup 26}Al ages in spite of their different oxygen isotopes, indicating that chondrule formed in the localized environment. The {sup 26}Al ages of chondrules in each chondrite class show a hint of correlation with their chemical compositions, which implies the process of elemental fractionation during chondrule formation events.
98 citations
TL;DR: In this paper, major, minor, and trace-element compositions for eleven Al-rich chondrules from unequilibrated ordinary chondrites were measured to investigate the relationships between Al-Rich chondrule, ferromagnesian chond rules, Ca-, Alrich inclusions (CAIs), and amoeboid olivine aggregates (AOAs).
79 citations
TL;DR: In this article, the sulfur isotopic compositions of putative primary troilite grains within 15 ferromagnesian chondrules (10 FeO-poor and 5 FeOrich chondrites) have been measured by ion microprobe.
63 citations
TL;DR: In this article, the authors measured oxygen and silicon isotopic compositions and Mn-Cr systematics in Fayalite from two petrographic settings of the Kaba meteorite.
44 citations
01 Dec 2005
TL;DR: In this paper, the potential genetic relationships between chondritic meteorites are evaluated and it is shown that in order to evaluate possible genetic relationships, it is necessary to understand and control the effects of parent body processing and secondary processes in the nebula.
Abstract: Chondrules, fine-grained rims on chondrules and CAIs, and fine-grained matrix are three major components of chondritic meteorites. In this chapter, we attempt to evaluate the potential genetic relationships between these components. We show that in order to evaluate possible genetic relationships, it is necessary to understand and control for the effects of parent body processing and secondary processes in the nebula. The meteorites best suited for this type of study are CO3.0, CR2, LL3.03.1, and some ungrouped chondrites such as Acfer 094 and Adelaide. We review petrographic, mineralogical, and compositional data for matrix and fine-grained rims and compare their characteristics to those of chondrules and bulk meteorites. Evidence is presented that can be interpreted to indicate that for each meteorite class, precursors for chondrules and matrix were exposed to the same thermal processing in the nebula and that chondrules and matrix are closely related. However, the evidence can also be interpreted in other ways that do not require a close relationship. We find that chondrules almost certainly lost volatiles through evaporation when they formed, but it is difficult to demonstrate the degree of loss. It is also difficult to determine the level to
44 citations
TL;DR: Extended abstract of a paper presented at Microscopy and Microanalysis 2005 in Honolulu, Hawaii, USA, July 31-August 4, 2005 as mentioned in this paper, presented by as mentioned in this paper.
Abstract: Extended abstract of a paper presented at Microscopy and Microanalysis 2005 in Honolulu, Hawaii, USA, July 31--August 4, 2005
1 citations