Ed:
This excerpt was taken from
http://www.lpi.usra.edu/meetings/lpsc97/pdf/1342.PDF, "Esquel:
Implications for Pallasite Formation Processes Based on the Petrography
of a Large Slab"
by Ulff-Moller, F.
<http://adsabs.harvard.edu/cgi-bin/author_form?author=Ulff-Moller,+F&fullauthor=Ulff-Moller,%20F.&charset=UTF-8&db_key=AST>;
Tran, J.
<http://adsabs.harvard.edu/cgi-bin/author_form?author=Tran,+J&fullauthor=Tran,%20J.&charset=UTF-8&db_key=AST>;
Choi, B.-G.
<http://adsabs.harvard.edu/cgi-bin/author_form?author=Choi,+B&fullauthor=Choi,%20B.-G.&charset=UTF-8&db_key=AST>;
Haag, R.
<http://adsabs.harvard.edu/cgi-bin/author_form?author=Haag,+R&fullauthor=Haag,%20R.&charset=UTF-8&db_key=AST>;
Rubin, A. E.
<http://adsabs.harvard.edu/cgi-bin/author_form?author=Rubin,+A&fullauthor=Rubin,%20A.%20E.&charset=UTF-8&db_key=AST>;
Wasson, J. T., 1997
<http://adsabs.harvard.edu/cgi-bin/author_form?author=Wasson,+J&fullauthor=Wasson,%20J.%20T.&charset=UTF-8&db_key=AST>
It summarizes how the Esquel parent body may have formed, resulting in a
beautiful meteorite when slabbed. Granted, this is not Krasnojarsk, but
it probably formed in a similar way.
"The largest slab available is that of Esquel
(belonging to Haag); the slab is ~90´36 cm
(surface area ~2900 cm2). Olivine is
volumetrically the most abundant phase;
angular grains range from submillimeter size
to 2.5 cm. Approximately 25 vol.% of the
olivine occurs in compact subrounded to
subangular masses ranging from 3´7 cm to
10´17 cm. The large olivine masses are
transected by thin veins of metallic Fe-Ni;
these veins presumably formed by the high pressure
injection of low-viscosity metal,
probably during an impact event. The large
olivine masses are probably fragments of
much larger (>>1 m) blocks from the mantle.
It seems likely that most of the small olivine
fragments were also produced during the
original crushing event, but we cannot rule
out a role by subsequent events. There are
relatively few olivine grains having sizes <1
mm and these tend to occur together in
patches; these may record late events
because the fine particles produced during
the initial crushing event may have been
consumed during (very limited)
recrystallization. There is no clear-cut
evidence of flow of the metallic liquid based
on the orientations of the individual olivine
grains."
E.P. Grondine wrote:
Hi all -
Sorry for a second post on this meteorite, but...
This is a wonderful slicing job by someone.
The contrasts in its components make this meteorite
remarkable. How did it form? There must have been
great temperature contrasts, and the materials are so
well separated. It would be nice to have microscopic
images of the boundaries.
great meteorite, but unfortunately I'd rather have a
new used car...
good hunting,
Ed
Man and Impact in the Americas
--- [EMAIL PROTECTED] wrote:
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Mile High Meteorites
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