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在ⅣB 群、ⅢAB 群和异常群铁陨石中,发现了~(107)Ag/~(109)Ag 比值的异常。过量的~(107)Ag(~(107)Ag~#)据推断是早期太阳系中~(107)Pd 衰变的结果。在高 Pd/Ag 比值和低 Ag 含量的样品中,Kaiser 和Wasserburg(1933)发现了过量的~(109)Ag。他们推断这些陨石中的~(109)Ag 是在极强的太阳耀斑的持续阶段中行星表面附近的~(108)Pd 受次级中子辐射的结果。这种粒子辐射必定持续到小行星体形成之后。~(107)Pd 可能是来源于银河系核合成的晚期阶段,或者是早期行星形成之前即太阳为金牛 T 型变星阶段时在太阳系内的局部产物。在最近的研究中,为了确定
Anomalies of ~ (107) Ag / ~ (109) Ag ratios were found in IVB, IIIAB and abnormal group iron meteorites. Excess Ag ~ (107) Ag ~ # is estimated to be the result of ~ (107) Pd decay in the early solar system. In samples with high Pd / Ag ratio and low Ag content, Kaiser and Wasserburg (1933) found excessive 109 Ag. They conclude that the (109) Ag in these meteorites is the result of the secondary neutron radiation of 108 Pd near the surface of the planet in the sustained phase of a very strong solar flare. This particle radiation must continue after the asteroid body is formed. ~ (107) Pd may originate from the late stage of galactic nuclear synthesis or may be a local product in the solar system before the formation of the early planet, that is, the sun is the Taurus T-stage variable star stage. In recent research, in order to determine