Chondrules and the Protoplanetary Disk

By E. Scott. 2011

328 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Ecology

View Paper: https://www.semanticscholar.org/paper/331e04f15f7b7520067172e88d5b83dac1dd66f5

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In Astronomy and Astrophysics

1. Lucio Mayer
2. R. Durisen
3. T. Hayfield
4. Aaron C. Boley
5. N. Movshovitz
6. Denton S. Ebel
7. E. Asphaug
8. M. Jutzi

In Ecology

1. Denton S. Ebel

Citations in the corpus

• Chondrule formation during planetesimal accretion (2011, background): “Chondrites consist predominately of ~ 0.1-1 mm igneous silicate spherules known as chondrules (e.g. Hewins et al., 1996; Ringwood, 1961; Scott, 2007; Scott and Krot, 2005; Sears, 2004; Sorby, 1864; Urey, 1967; Wood, 1963).”
• Clumps in the outer disk by disk instability: Why they are initially gas giants and the legacy of disruption (2009, background): “ial or entire, may be a mechanism for processing Calcium-AluminiumInclusions (CAIs) or CAI-like particles. CAIs are composed of refractory minerals that are stable at temperatures above 1400 K (e.g., Scott 2007). The advantage of this formation mechanism is that it can occur as soon as the disk begi”
• Chondrule size and related physical properties: a compilation and evaluation of current data across all meteorite groups (2014, background): “rocessing. Chondrules can also be grouped by their composition: Type I (low FeO and moderately volatile element poor) and Type II (high FeO content and less depleted in moderately volatile elements) (Hewins et al., 1996). In an abstract, Haack and Scott (1993) stated that type I chondrules are small”