[meteorite-list] Meteorite Evidence for the Accretion and Collisional Evolution of Asteroids---- Good Read

From: Shawn Alan <photophlow_at_meteoritecentral.com>
Date: Fri, 15 Oct 2010 18:36:04 -0700 (PDT)
Message-ID: <299940.42886.qm_at_web35404.mail.mud.yahoo.com>

Hello Lister,
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Here is a great paper on the break down of classifications of meteorites by type and which parent bodies they come from. I have read about 6 pages so far and liked the descriptions they give for each section and how paper has it all in one place. Also its always interesting to learn where?meteorite originate from and what their parent bodies might be like.?Check it out and its an easy read and good resource to have.
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Meteorite Evidence for the Accretion and
Collisional Evolution of Asteroids

Edward R. D. Scott
University of Hawai?i

Meteorites contain a record of impacts during all stages of asteroid origin and evolution:
the formation and accretion of chondritic particles; the alteration, metamorphism and melting
of asteroids; and the erosion and disruption of asteroids by hypervelocity impacts. A review of
meteorite classification shows that numerous meteorites are not readily classified because they
do not fit simple models for asteroid formation and evolution that assume impacts were only
important during the final stage of asteroid evolution and because of inadequate understanding
of asteroidal impacts. Chronological, textural, and thermal constraints allow us to identify meteorite
impact breccias that formed during accretion (e.g., Kaidun), when asteroids were partly
molten (e.g., mesosiderites), and during the subsequent disruption of asteroids (e.g., L chondrites).
Studies of chondrites including Kaidun suggest that chondrules accreted with similarsized
fragments of preexisting bodies that formed at greater heliocentric distances. In the inner
solar system, chondrules appear to have been crucial for initiating accretion. Without chondrules
and rock fragments, dry dust failed to accrete to the nebular midplane because of nebular
turbulence and spiraled into the protosun. The tiny mass of asteroids may be partly due to
inefficient chondrule formation beyond 2 AU or less-efficient delivery of chondrules from near
the protosun.

http://www.higp.hawaii.edu/~escott/Asteroid%20III.pdf

Shawn Alan
IMCA 1633
eBaystore
http://shop.ebay.com/photophlow/m.html?_nkw=&_armrs=1&_from=&_ipg=&_trksid=p4340
Received on Fri 15 Oct 2010 09:36:04 PM PDT