A short duration of chondrule formation in the solar nebula: evidence from 26Al in Semarkona ferromagnesian chondrules

Kita, N. T.; Nagahara, H.; Togashi, S.; Morishita, Y.

doi:10.1016/s0016-7037(00)00488-9

Cited by 205 publications

(249 citation statements)

References 29 publications

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“…27 Al/ 24 Mg ratios in plagioclase range from ~30 to ~260. A similar range of 27 Al/ 24 Mg ratios was reported in chondrule plagioclase from type 3 ordinary and CO carbonaceous chondrites (e.g., Kita et al, 2000;Kurahashi et al, 2008a). Six out of fourteen chondrules (4 of 7 Al-rich, 1 of 5 type I, and 1 of 2 type II chondrules) have apparent 26 Mg/ 24 Mg excesses (δ 26 Mg*) that are resolved at the 2σ level.…”

Section: Resultssupporting

confidence: 73%

“…3, together with the observed ranges (average ± 2SD) of ( 26 Al/ 27 Al) 0 in chondrules from the least metamorphosed chondrites, LL3.0 Semarkona, CO3.0 Yamato 81020, and ungrouped type 3 chondrite Acfer 094 (from Hutcheon and Hutchison, 1989;Kita et al, 2000;Kunihiro et al, 2004;Kurahashi et al, 2008a;Rudraswami et al, 2008;Villeneuve et al, 2009;Ushikubo et al, 2013 Hutcheon and Hutchison (1989), Kita et al (2000), Kunihiro et al (2004), Kurahashi et al (2008a), Rudraswami et al (2008), Villeneuve et al (2009), and Ushikubo et al (2013).…”

Section: Resultsmentioning

confidence: 60%

“…1 and S1). These plagioclase grains contain variable concentrations of MgO ranging ~0.2-1.6 wt%, similar to those in chondrule plagioclase from unmetamorphosed chondrites (e.g., Kita et al, 2000;Krot et al, 2002;Kurahashi et al, 2008a). A type II chondrule, GRA 95229-31-#72, has lath-shaped Na-rich plagioclase An [43][44][45][46][47][48][49] (Table 1, Fig.…”

Section: Resultsmentioning

confidence: 97%

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<sup>26</sup>Al in chondrules from CR2 chondrites

2014

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Section: Resultssupporting

confidence: 73%

Section: Resultsmentioning

confidence: 60%

Section: Resultsmentioning

confidence: 97%

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<sup>26</sup>Al in chondrules from CR2 chondrites

2014

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“…Thermal metamorphism is responsible for the partial destruction of the primary mineral textures and the growth of secondary mineral. On the basis of Al-Mg isotopic data, it was found that the metamorphism of chondritic parent body occurred a few million years after the formation of CAIs (Kita et al 2000;Huss et al 2001).…”

Section: Evolution Of the Solar Systemmentioning

confidence: 99%

Meteorites: Rocks From the Outer Space

Doh¹,

2010

Journal of The Korean Astronomical Society

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According to the historical documents and paintings in many civilizations, rocks that fell from the sky fascinated humans as the message from the God or supernaturals. Scientific progress allows humans to recognize these exciting extraterrestrial objects as meteorites. Meteorites contain a wealth of pivotal information regarding formation of the early Solar System. Meteorites also provide broader scientific insights on, for example, the origin of life, interplanetary transfer of life forms, massive depletion of biosphere on Earth, and evolution of lithosphere on Earth-like planetary bodies.

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“…In addition, radioisotope dating of the most primitive chondrites supports that the formation of chondrules began at least a million years after the formation of the Solar nebula (e.g. Kita et al 2000Kita et al , 2005. This also suggests that the dust growth process towards planetesimals is "inefficient" (Cuzzi et al 2008).…”

mentioning

confidence: 98%

Electrostatic Barrier Against Dust Growth in Protoplanetary Disks. Ii. Measuring the Size of the “Frozen” Zone

Okuzumi

Tanaka

Takeuchi

et al. 2011

ApJ

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Coagulation of submicron-sized dust grains into porous aggregates is the initial step of dust evolution in protoplanetary disks. Recently, it has been pointed out that negative charging of dust in the weakly ionized disks could significantly slow down the coagulation process. In this paper, we apply the growth criteria obtained in Paper I to finding out a location ("frozen" zone) where the charging stalls dust growth at the fractal growth stage. For low-turbulence disks, we find that the frozen zone can cover the major part of the disks at a few to 100 AU from the central star. The maximum mass of the aggregates is approximately 10 −7 g at 1 AU and as small as a few monomer masses at 100 AU. Strong turbulence can significantly reduce the size of the frozen zone, but such turbulence will cause the fragmentation of macroscopic aggregates at later stages. We examine a possibility that complete freezeout of dust evolution in low-turbulence disks could be prevented by global transport of dust in the disks. Our simple estimation shows that global dust transport can lead to the supply of macroscopic aggregates and the removal of frozen aggregates on a timescale of 10 6 yr. This overturns the usual understanding that tiny dust particles get depleted on much shorter timescales unless collisional fragmentation is effective. The frozen zone together with global dust transport might explain "slow" (∼ 10 6 yr) dust evolution suggested by infrared observation of T Tauri stars and by radioactive dating of chondrites.

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A short duration of chondrule formation in the solar nebula: evidence from 26Al in Semarkona ferromagnesian chondrules

Cited by 205 publications

References 29 publications

<sup>26</sup>Al in chondrules from CR2 chondrites

<sup>26</sup>Al in chondrules from CR2 chondrites

Meteorites: Rocks From the Outer Space

Electrostatic Barrier Against Dust Growth in Protoplanetary Disks. Ii. Measuring the Size of the “Frozen” Zone

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