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Quenching of the SnSbTe Cycle in the rp Process

Journal Article · · Physical Review Letters
; ; ; ; ; ; ; ; ; ; ;  [1]; ; ;  [2]; ; ;  [2];  [3]
  1. Department of Physics, University of Jyvaeskylae, Post Office Box 35, FI-40014 (Finland)
  2. Petersburg Nuclear Physics Institute, 188300 Gatchina (Russian Federation)
  3. Department of Physics and Astronomy, National Superconducting Cyclotron Laboratory, and Joint Institute for Nuclear Astrophysics, Michigan State University, East Lansing, Michigan 48824 (United States)
The nuclides {sup 104-108}Sn, {sup 106-110}Sb, {sup 108,109}Te, and {sup 111}I at the expected endpoint of the astrophysical rp process have been produced in {sup 58}Ni+{sup nat}Ni fusion-evaporation reactions at IGISOL and their mass values were precisely measured with the JYFLTRAP Penning trap mass spectrometer. For {sup 106}Sb, {sup 108}Sb, and {sup 110}Sb these are the first direct experimental mass results obtained. The related one-proton separation energies have been derived and the value for {sup 106}Sb, S{sub p}=424(8) keV, shows that the branching into the closed SnSbTe cycle in the astrophysical rp process is weaker than expected.
OSTI ID:
21346996
Journal Information:
Physical Review Letters, Journal Name: Physical Review Letters Journal Issue: 25 Vol. 102; ISSN 0031-9007; ISSN PRLTAO
Country of Publication:
United States
Language:
English