On Search and Identification of Super Heavy (Z = 110 - 114) and Super Super Heavy (Z Greater Than or Equal To 160) Cosmic Ray Nuclei Tracks in the Moon Olivine Crystals

Details On Search and Identification of Super Heavy (Z = 110 - 114) and Super Super Heavy (Z Greater Than or Equal To 160) Cosmic Ray Nuclei Tracks in the Moon Olivine Crystals On Search and Identification of Super Heavy (Z = 110 - 114) and Super Super Heavy (Z Greater Than or Equal To 160) Cosmic Ray Nuclei Tracks in the Moon Olivine Crystals

Jan 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002mbns.conf...45p&link_type=abstract

The Moon Beyond 2002: Next Steps in Lunar Science and Exploration, p. 45

Physics

Cosmic Rays, Nuclei, Olivine, Lunar Surface, Fossils, Electromagnetic Fields, Neutron Stars

Scientific paper

The main goal of the present work is the search and possible identification of relatively stable nuclei of Super Heavy (Z=110 - 114)(SHE) and Super Super Heavy (Z= 160) elements (SSHE) in Galactic cosmic rays, basing on the fossil track studies of the olivine crystals from the Moon surface. Nuclei of the elements with Z more than or equal to 30 up to Th - U and Z = 110-160 are most probably the products of Supernova explosion when freshly formed neutron star matter erupted outside (about 10% of its final mass). That neutron matter supposed to be then degraded. It is thought to be the main source of all the heaviest element in the Galaxy. The strong nonpermanent electromagnetic fields of exploding star can provide the acceleration of these freshly formed nuclei up to energies 10 6 MeV per nuclon.

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