Interstellar 60Fe on the Surface of the Moon

被引:101
作者
Fimiani, L. [1 ]
Cook, D. L. [2 ,4 ]
Faestermann, T. [1 ]
Gomez-Guzman, J. M. [1 ]
Hain, K. [1 ]
Herzog, G. [2 ]
Knie, K. [1 ,5 ]
Korschinek, G. [1 ]
Ludwig, P. [1 ]
Park, J. [2 ]
Reedy, R. C. [3 ]
Rugel, G. [1 ,6 ]
机构
[1] Tech Univ Munich, Dept Phys, D-85748 Garching, Germany
[2] Rutgers State Univ, Dept Chem & Chem Biol, Piscataway, NJ 08854 USA
[3] Planetary Sci Inst, Los Alamos, NM 87544 USA
[4] ETH, CH-8092 Zurich, Switzerland
[5] GSI Darmstadt, Planckstr 1, D-64291 Darmstadt, Germany
[6] Helmholtz Zentrum Dresden Rossendorf, D-01314 Dresden, Germany
关键词
HALF-LIFE; MASSIVE STARS; NUCLEOSYNTHESIS; BE-10; MN-53; EARTH; GAS; AMS;
D O I
10.1103/PhysRevLett.116.151104
中图分类号
O4 [物理学];
学科分类号
0702 ;
摘要
A dying massive star ends in a supernova explosion ejecting a large fraction of its mass into the interstellar medium. If this happens nearby, part of the ejecta might end on Solar System bodies and, in fact, radioactive Fe-60 has been detected on the Pacific ocean floor in about 2 Ma old layers. Here, we report on the detection of this isotope also in lunar samples, originating presumably from the same event. The concentration of the cosmic ray produced isotope Mn-53, measured in the same samples, proves the supernova origin of the Fe-60. From the Fe-60 concentrations found we deduce a reliable value for the local interstellar fluence in the range of 1 x 10(8) at/cm(2). Thus, we obtain constraints on the recent and nearby supernova(e).
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页数:5
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