The Rumuruti chondrite group

Bischoff, A.; Vogel, N.; Roszjar, J.

doi:10.1016/j.chemer.2011.02.005

Cited by 113 publications

(174 citation statements)

References 106 publications

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“…2003). Also, all chondrite groups contain a small abundance of Al‐rich chondrules (e.g., Bischoff and Keil 1983, 1984; Bischoff et al. 1985, 1989, 1994, 2011; Rout and Bischoff 2008; Rout et al.…”

Section: Resultsmentioning

confidence: 99%

Macrochondrules in chondrites—Formation by melting of mega‐sized dust aggregates and/or by rapid collisions at high temperatures?

Weyrauch

Bischoff

2012

Meteorit & Planetary Scien

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Abstract-Seventy-four macrochondrules with sizes >3 mm were studied. Considering the extraordinary size of the chondrules (occasionally achieving a mass of 1000 times (and more) the mass of a normal-sized chondrule), the conditions in the formation process must have been somewhat different compared with the conditions for the formation of the common chondrules. Macrochondrules are typically rich in olivine and texturally similar to specific chondrule types (barred, radial, porphyritic, and cryptocrystalline) of normal-sized chondrules. However, our studies show that most of the macrochondrules are fine-grained or have elongated crystals (mostly BO, RP, and C), which lead to the assumption that they were once totally molten and cooled quite rapidly. Porphyritic chondrules belong to the least abundant types of macrochondrules. This distribution of chondrule types is highly unusual and just a reverse of the distribution of chondrule types among the typical-sized chondrules in most chondrite groups except for the CH and CB chondrites. New chondrule subtypes (like radialolivine [RO] or multi-radial [MR] chondrules) are defined to better describe the textures of certain large chondrules. Macrochondrules may have formed due to melting of huge precursor dust aggregates or due to rapid collisions of superheated melt droplets, which led to the growth of large molten spherules in regions with high dust densities and high electrostatic attraction.

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Section: Resultsmentioning

confidence: 99%

Macrochondrules in chondrites—Formation by melting of mega‐sized dust aggregates and/or by rapid collisions at high temperatures?

Weyrauch

Bischoff

2012

Meteorit & Planetary Scien

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“…2D) is unique. It shows many characteristics typical of R chondrites but has higher abundances of metal compared with typical R chondrites (Bischoff et al 2011). …”

Section: Chondritesmentioning

confidence: 97%

Asteroid 2008 TC3 and the Fall of Almahata Sitta, a Unique Meteorite Breccia

Goodrich

Bischoff²,

O’Brien

2014

Elements

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“…For the monomineralic-olivine asteroids they found olivine chemistries in the range of Fa 30-51 , consistent with both brachinites and R chondrites. Olivine-rich asteroids, on the other hand, showed spectral characteristics similar to those of R chondrites, with olivine abundances ranging from 68% to 78% (Bischoff et al, 2011). Interestingly, several of the objects studied by Sanchez et al (2014) are located at $2.8 AU from the Sun, near the 5:2 mean motion resonance with Jupiter.…”

Section: Mixturesmentioning

confidence: 86%