Abstract
Harris and Tozer1 have recently suggested that magnetostatic attraction between cosmic iron particles is responsible for the observed variation in iron abundance between the inner and outer planets of the solar system. I should like to point out that a crucial assumption in this model is “the uniform single-domain nature” of iron particles in the size range 10−4–10−3 cm. The calculations which follow show that iron particles of only a limited size range can take part in magnetostatic accretion.
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References
Harris, P. G., and Tozer, D. C., Nature, 215, 1449 (1967).
Morrish, A. H., in The Physical Principles of Magnetism, 340 (John Wiley and Sons, 1965).
Kittel, C., in Introduction to Solid State Physics, 430 (John Wiley and Sons, 1957).
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BANERJEE, S. Fractionation of Iron in the Solar System. Nature 216, 781 (1967). https://doi.org/10.1038/216781a0
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DOI: https://doi.org/10.1038/216781a0
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