Other
Scientific paper
Sep 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990gecoa..54.2577z&link_type=abstract
Geochimica et Cosmochimica Acta (ISSN 0016-7037), vol. 54, Sept. 1990, p. 2577-2586.
Other
5
Planetary Evolution, Porous Materials, Protoplanets, Xenon, Carbonaceous Meteorites, Earth (Planet), Mars (Planet), Solar System
Scientific paper
The distinctively fractionated Xe on Mars and earth may have its root in a common source from which both planets accreted. Beginning with Ozima and Nakazawa's (1980) hypothesis that terrestrial Xe fractionation was caused by gravitational separation of adsorbed solar nebular gases inside large porous planetesimals, it is pointed out that Xe would have been trapped as the planetesimal grew and pores were squeezed shut by lithostatic pressure. It is shown that enough fractionated Xe to supply the earth could have been trapped this way. The degree of fractionation is controlled by the lithostatic pressure at the pore-closing front and so would have been roughly the same for all large planetesimals. The predicted degree of fractionation agrees well with that preserved in terrestrial and Martian Xe. Relative to Xe, this source is strongly depleted in other noble gases. In contrast to the original Ozima and Nakazawa hypothesis, the present hypothesis predicts the observed fractionation, and it allows planetary accretion to occur after the dissipation of the solar nebula.
Kasting James F.
Pollack James B.
Zahnle Kevin
No associations
LandOfFree
Xenon fractionation in porous planetesimals does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Xenon fractionation in porous planetesimals, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Xenon fractionation in porous planetesimals will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1404213