Meteoritic parent bodies: Their number and identification

By T. Burbine, T. Mccoy, A. Meibom, B. Gladman, K. Keil. 2002

261 citations recorded by the source corpus.

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Citations in the corpus

Differentiated Planetesimals and the Parent Bodies of Chondrites (2013, background): “…SHE, shergottites; URE, ureilites; IR, infrared; V, visible. are: (a) The meteorite suite is not representative of the present-day asteroid belt (Burbine et al. 2002); (b) few large, differentiated asteroids have survived to the present day (Bottke et al. 2006); or (c) some asteroid spectral…”
Linking the collisional history of the main asteroid belt to its dynamical excitation and depletion (2005, background): “(For a recent review of the number of parent bodies represented in our meteorite record, see Burbine et al., 2002.)”
Chondrules and the Protoplanetary Disk (2011, background): “In addition, igneously differentiated asteroids, besides Vesta, appear to be rare (Burbine et al. 2002). www.annualreviews.org • Chondrites and the Protoplanetary Disk 603 A nn u.”
Gravitational Aggregates: Evidence and Evolution (2002, background): “Chandrasekhar, 1969) implies, for example, that a body with a bulk density of 2 g cm–3 and no tensile strength can be disrupted if it passes within 3.4 R of Earth’s center, where R is Earth’s radius. The Roche limit in general applies only to synchronous rotating liquid satellites in circular orbit.”
The Compositional Structure of the Asteroid Belt (2015, background): “ Question B2). Assuming that a group comes from a single parent body and that ungrouped meteorites come from separate parent bodies, meteorites appear to be samples of 100-150 distinct parent bodies (Burbine et al., 2002; Appendix Question B1). Chondrites The chondrites are composed of three major c”
Origin of water in the inner Solar System: Planetesimals scattered inward during Jupiter and Saturn's rapid gas accretion (2017, background): “Asteroid classes have been spectroscopically associated with different types of meteorites (Burbine et al., 2002).”
SPACE WEATHERING OF ASTEROID SURFACES (2004, background): “Probably, such parent bodies are among the S-type asteroids (Burbine et al. 2002), especially those that deviate greatly from S(IV) characteristics in the band-area-ratio/band-center relationship of Gaffey et al. (1993).”
Hydrated Minerals on Asteroids: The Astronomical Record (2003, background): “5 μm in some E asteroids may be due to troilite (FeS) or other sulfides, and that the mineral responsible may also be responsible for the 3-μm feature in E-class and perhaps M-class asteroids. If true, this would potentially allow S contents of these asteroids to be determined, and would strengthen ”
In search of the source of asteroid (101955) Bennu: Applications of the stochastic YORP model (2015, background): “, 2012), carbonaceous chondrite meteorites only provide <3% of all meteorite falls (Burbine et al., 2002).”
Populating the asteroid belt from two parent source regions due to the migration of giant planets—“The Grand Tack” (2012, background): “However, this is not to imply that there are only two specific types of asteroids—rather compositional variations within each group would account for a large variety of asteroid taxonomic classes and meteorite groups (Burbine et al. 2002; Bus et al. 2002; DeMeo et al. 2009).”
Density of asteroids (2012, background): “Other regions of the Solar System may therefore be unrepresented in our meteorite collection (see the discussions in, Burbine et al., 2002; Bottke et al., 2002b; Vernazza et al., 2008, for instance).”
Melting and differentiation of early-formed asteroids: The perspective from high precision oxygen isotope studies (2017, methodology): “The Howardite, Eucrite, Diogenite suite (HEDs) is the most abundant group of differentiated meteorites arriving on Earth today, comprising roughly 6% of all witnessed falls (statistics from Mete- oritical Bulletin Database; see also Burbine et al., 2002a).”