Abstract
Meteorites may be pieces of main-belt asteroids, derived by cratering collisions. The physical strength of an asteroid critically affects the quantity of ejecta that can be placed in orbits (probably resonant) that evolve to cross the Earth's. Asteroid strengths very widely due to initial composition and size (e.g., weak carbonaceous material or strong rock), subsequent geophysical evolution (e.g., formation of a strong iron core), and subsequent collisional evolution (e.g., conversion of a strong rocky body into a weak rubble pile). The meteorite yield on Earth further depends on meteorite strength, which affects longevity in space and survival through the atmosphere. We show that meteorites may be derived mainly by cratering rather than by disruptive fragmentation and from large main-belt asteroids rather than from small, Earth-approaching bodies. The model combines a wide variety of evidence from various disciplines to yield results consistent with meteorite statistics. However, no claim is made for uniqueness of this model, and many elements still admit considerable uncertainty.
| Original language | English (US) |
|---|---|
| Pages (from-to) | 455-481 |
| Number of pages | 27 |
| Journal | Icarus |
| Volume | 55 |
| Issue number | 3 |
| DOIs | |
| State | Published - 1983 |
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ASJC Scopus subject areas
- Space and Planetary Science
- Astronomy and Astrophysics
Cite this
Asteroids and meteorites : Parent bodies and delivered samples. / Greenberg, Richard J.; Chapman, Clark R.
In: Icarus, Vol. 55, No. 3, 1983, p. 455-481.Research output: Contribution to journal › Article
}
TY - JOUR
T1 - Asteroids and meteorites
T2 - Parent bodies and delivered samples
AU - Greenberg, Richard J.
AU - Chapman, Clark R.
PY - 1983
Y1 - 1983
N2 - Meteorites may be pieces of main-belt asteroids, derived by cratering collisions. The physical strength of an asteroid critically affects the quantity of ejecta that can be placed in orbits (probably resonant) that evolve to cross the Earth's. Asteroid strengths very widely due to initial composition and size (e.g., weak carbonaceous material or strong rock), subsequent geophysical evolution (e.g., formation of a strong iron core), and subsequent collisional evolution (e.g., conversion of a strong rocky body into a weak rubble pile). The meteorite yield on Earth further depends on meteorite strength, which affects longevity in space and survival through the atmosphere. We show that meteorites may be derived mainly by cratering rather than by disruptive fragmentation and from large main-belt asteroids rather than from small, Earth-approaching bodies. The model combines a wide variety of evidence from various disciplines to yield results consistent with meteorite statistics. However, no claim is made for uniqueness of this model, and many elements still admit considerable uncertainty.
AB - Meteorites may be pieces of main-belt asteroids, derived by cratering collisions. The physical strength of an asteroid critically affects the quantity of ejecta that can be placed in orbits (probably resonant) that evolve to cross the Earth's. Asteroid strengths very widely due to initial composition and size (e.g., weak carbonaceous material or strong rock), subsequent geophysical evolution (e.g., formation of a strong iron core), and subsequent collisional evolution (e.g., conversion of a strong rocky body into a weak rubble pile). The meteorite yield on Earth further depends on meteorite strength, which affects longevity in space and survival through the atmosphere. We show that meteorites may be derived mainly by cratering rather than by disruptive fragmentation and from large main-belt asteroids rather than from small, Earth-approaching bodies. The model combines a wide variety of evidence from various disciplines to yield results consistent with meteorite statistics. However, no claim is made for uniqueness of this model, and many elements still admit considerable uncertainty.
UR - http://www.scopus.com/inward/record.url?scp=0000624259&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=0000624259&partnerID=8YFLogxK
U2 - 10.1016/0019-1035(83)90116-1
DO - 10.1016/0019-1035(83)90116-1
M3 - Article
AN - SCOPUS:0000624259
VL - 55
SP - 455
EP - 481
JO - Icarus
JF - Icarus
SN - 0019-1035
IS - 3
ER -