Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1972
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1972ap%26ss..15..214g&link_type=abstract
Astrophysics and Space Science, Volume 15, Issue 2, pp.214-228
Astronomy and Astrophysics
Astrophysics
24
Scientific paper
Relative abundances in the region 74≤Z≤83 (W to Bi) are determined for 73 Dra, HR 4072, and some other Ap stars. Abundance peaks occur at atomic massesA=191±2 on 73 Dra, atA=201±3 on HR 4072, atA=199±5 on other ‘main’ group Ap stars, and atA=201±2 on Mn stars. Pb has a relatively low abundance on Ap stars and also in cosmic rays which have an abundance peak atA=193±3. The abundance peaks on ‘main’ group Ap stars are due to the cyclicr-process which occurred in explosions of former companion stars. Fission products of transuranic elements are recycled by further rapid neutron captures. At the end of ther-process, the high neutron flux decreases gradually so that the final β-decays take place in a neutron-rich environment; superheavy elements (Z≥110) formed in ther-process may be partly destroyed by neutron-induced fission. The pulsar remnants of the explosions accelerater-process elements to cosmic-ray energies. The peak atA ˜ 201 on Mn stars is discussed briefly.
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