Cameron 1963

Cameron, A.G.W., 1963: The origin of atmospheric xenon. Icarus, 1, 314-316, doi:10.1016/0019-1035(62)90029-5.

Part of the differences in isotopic composition of atmospheric and meteoritic xenon can be attributed to irradiation of solar xenon by neutrons during the deuterium-burning phase of solar contraction, followed by accretion of the irradiated xenon into the atmosphere. This problem is examined here more carefully following a new measurement of the reaction rate for capture of protons by deuterium by Griffiths, Lal, and Scorfe. It is concluded that the majority of atmospheric xenon, apart from that produced by the decay of extinct radioactivities, was once in the Sun during the deuterium-burning phase.

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Cameron, A.G.W.: The origin of atmospheric xenon, Icarus, 1, 314-316, doi:10.1016/0019-1035(62)90029-5, 1963.

Cameron, A.G.W. (1963), The origin of atmospheric xenon, Icarus, 1, 314-316, doi:10.1016/0019-1035(62)90029-5.

Cameron, A.G.W., 1963: The origin of atmospheric xenon. Icarus, 1, 314-316, doi:10.1016/0019-1035(62)90029-5.

Cameron, A.G.W. 1963, Icarus, 1, 314, doi:10.1016/0019-1035(62)90029-5.

Cameron AGW. The origin of atmospheric xenon, Icarus 1963;1:314-316. doi:10.1016/0019-1035(62)90029-5.

A.G.W. Cameron, Icarus 1, 314-316, doi:10.1016/0019-1035(62)90029-5 (1963).