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Phys. Rev. Lett. 102, 252501 (2009) [4 pages]

Quenching of the SnSbTe Cycle in the rp Process

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V.-V. Elomaa1,*, G. K. Vorobjev2,3, A. Kankainen1, L. Batist2, S. Eliseev2,3,†, T. Eronen1, J. Hakala1, A. Jokinen1, I. D. Moore1, Yu. N. Novikov2,3, H. Penttilä1, A. Popov2, S. Rahaman1,‡, J. Rissanen1, A. Saastamoinen1, H. Schatz4, D. M. Seliverstov2, C. Weber1,§, and J. Äystö1
1Department of Physics, University of Jyväskylä, Post Office Box 35, FI-40014, Finland
2Petersburg Nuclear Physics Institute, 188300 Gatchina, Russia
3Gesellschaft für Schwerionenforschung mbH, Planckstraße 1, D-64291 Darmstadt, Germany
4Department of Physics and Astronomy, National Superconducting Cyclotron Laboratory, and Joint Institute for Nuclear Astrophysics, Michigan State University, East Lansing, Michigan 48824, USA

Received 17 February 2009; published 25 June 2009

The nuclides 104–108Sn, 106–110Sb, 108,109Te, and 111I at the expected endpoint of the astrophysical rp process have been produced in 58Ni+natNi fusion-evaporation reactions at IGISOL and their mass values were precisely measured with the JYFLTRAP Penning trap mass spectrometer. For 106Sb, 108Sb, and 110Sb these are the first direct experimental mass results obtained. The related one-proton separation energies have been derived and the value for 106Sb, Sp=424(8)  keV, shows that the branching into the closed SnSbTe cycle in the astrophysical rp process is weaker than expected.

© 2009 The American Physical Society

URL:
http://link.aps.org/doi/10.1103/PhysRevLett.102.252501
DOI:
10.1103/PhysRevLett.102.252501
PACS:
21.10.Dr, 26.30.−k, 26.50.+x, 27.60.+j

*viki-veikko.v.elomaa@jyu.fi

Present address: Max-Planck-Institut für Kernphysik, D-69117 Heidelberg, Germany.

Present address: Physics Division, P-23, Mail Stop H803, Los Alamos National Laboratory, Los Alamos, NM 87545, USA.

§Present address: Fakultät für Physik, Ludwig-Maximilians-Universität München, Am Coulombwall 1, D-85748 Garching, Germany.