Role of gas-melt interaction during chondrule formation

Libourel, G.; Krot, Alexander N.; Tissandier, L.

doi:10.1016/j.epsl.2006.09.011

Cited by 145 publications

(195 citation statements)

References 25 publications

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“…5). The composition of the CMAS glass (G B = 24.09 wt% CaO,6.44 wt% MgO, 29.65 wt% Al 2 O 3 and 39.77 wt% SiO 2 ) corresponds to the most Ca-Al-rich mesostasis composition of type IA chondrules measured in Semarkona (Jones and Scott, 1989), which can be interpreted as the composition of chondrules that interacted the least with the surrounding environment during their formation (Libourel et al, 2006). As shown in Table 1, C0 to C4 mixtures contain from 0 to 20 wt% of iron metal.…”

Section: Methodsmentioning

confidence: 99%

“…thermodynamic calculations relating the FeO content of the magnesian olivine to the oxygen fugacity (Nitsan, 1974;Matas et al, 2000) suggest that type I in Semarkona (Jones 37 and Scott, 1989;Libourel et al, 2006) formed in redox conditions in the range of 2 to 4 log units below the IW buffer curve (Fig. 3).…”

Section: Redox Conditions During Chondrule Formationmentioning

confidence: 99%

“…Alexander et al, 2000;Alexander and Wang, 2001;Yu et al, 2003;Lauretta et al, 2006;Alexander et al, 2008;Fedkin et al, 2012), (ii) metal grains in dusty olivines (Nipoor) and metal in type I chondrules (Ni-rich) do not have the same origin and thus could not have been formed simultaneously by an evaporation/reduction process (e.g. Rambaldi and Wasson, 1981;Leroux et al, 2003;Hewins et al, 2005), (iii) chemical gradients of volatiles and moderately volatiles elements in chondrule mesostasis and occurrence of mineralogical zoning in some chondrules argue in favor of condensation rather than evaporation processes (Matsunami et al, 1993;Nagahara et al, 1999;Libourel et al, 2003, Libourel et al, 2006Krot et al, 2004;Alexander et al , 2008;.…”

Section: Introductionmentioning

confidence: 99%

“…Sears et al, 1996;Hewins et al, 2005;Jones et al, 2005;Alexander et al, 2008;Alexander and Ebel, 2012;, a number of arguments based on chemical (e.g. Matsunami et al, 1993;Nagahara et al, 1999;Libourel et al, 2003;Libourel et al, 2006;Krot et al, 2004), isotopic (e.g. Thiemens, 1996;Clayton, 2004;Chaussidon et al, 2008;Libourel and Chaussidon, 2011) and experimental (e.g.…”

Section: Introductionmentioning

confidence: 99%

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Relationships between type I and type II chondrules: Implications on chondrule formation processes

Villeneuve

Libourel

Soulié

2015

Geochimica et Cosmochimica Acta

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Please cite this article as: Villeneuve, J., Libourel, G., Soulié, C., Relationships between type I and type II chondrules: Implications on chondrule formation processes, Geochimica et Cosmochimica Acta (2015), doi: http://dx.doi.org/ 10.1016/j.gca. 2015.03.033 This is a PDF file of an unedited manuscript that has been accepted for publication. As a service to our customers we are providing this early version of the manuscript. The manuscript will undergo copyediting, typesetting, and review of the resulting proof before it is published in its final form. Please note that during the production process errors may be discovered which could affect the content, and all legal disclaimers that apply to the journal pertain.

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Section: Methodsmentioning

confidence: 99%

Section: Redox Conditions During Chondrule Formationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Relationships between type I and type II chondrules: Implications on chondrule formation processes

Villeneuve

Libourel

Soulié

2015

Geochimica et Cosmochimica Acta

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“…Olivines first crystallized from the melt, and pyroxenes on the edge of the chondrules later formed by interaction of these olivines with protosolar SiO gas (e.g. [176,179,180]). The olivines in Type I chondrules frequently show triple junctions typical of textures observed in terrestrial mantle rocks, suggesting that Type I chondrules actually originate from the mantle of differentiated asteroids [176,177].…”

Section: -P12mentioning

confidence: 99%

Meteorites and cosmic dust: Interstellar heritage and nebular processes in the early solar system

Engrand

2011

EPJ Web of Conferences

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Abstract. Small solar system bodies like asteroids and comets have escaped planetary accretion. They are the oldest and best preserved witnesses of the formation of the solar system. Samples of these celestial bodies fall on Earth as meteorites and interplanetary dust. The STARDUST mission also recently returned to Earth cometary dust from comet 81P/Wild 2, a Jupiter Family Comet (JFC). These samples provide unique insights on the physico-chemical conditions and early processes of the solar system. They also contain some minute amount of materials inherited from the local interstellar medium that have survived the accretion processes in the solar system.

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Chondrules: The canonical and noncanonical views

Connolly

Jones

2016

JGR Planets

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Millimeter‐scale rock particles called chondrules are the principal components of the most common meteorites, chondrites. Hence, chondrules were arguably the most abundant components of the early solar system at the time of planetesimal accretion. Despite their fundamental importance, the existence of chondrules would not be predicted from current observations and models of young planetary systems. There are many different models for chondrule formation, but no single model satisfies the many constraints determined from their mineralogical and chemical properties and from chondrule analog experiments. Significant recent progress has shown that several models can satisfy first‐order constraints and successfully reproduce chondrule thermal histories. However, second‐ and third‐order constraints such as chondrule size ranges, open system behavior, oxidation states, reheating, and chemical diversity have not generally been addressed. Chondrule formation models include those based on processes that are known to occur in protoplanetary disk environments, including interactions with the early active Sun, impacts and collisions between planetary bodies, and radiative heating. Other models for chondrule heating mechanisms are based on hypothetical processes that are possible but have not been observed, like shock waves, planetesimal bow shocks, and lightning. We examine the evidence for the canonical view of chondrule formation, in which chondrules were free‐floating particles in the protoplanetary disk, and the noncanonical view, in which chondrules were the by‐products of planetesimal formation. The fundamental difference between these approaches has a bearing on the importance of chondrules during planet formation and the relevance of chondrules to interpreting the evolution of protoplanetary disks and planetary systems.

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Role of gas-melt interaction during chondrule formation

Cited by 145 publications

References 25 publications

Relationships between type I and type II chondrules: Implications on chondrule formation processes

Relationships between type I and type II chondrules: Implications on chondrule formation processes

Meteorites and cosmic dust: Interstellar heritage and nebular processes in the early solar system

Chondrules: The canonical and noncanonical views

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