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Phys. Rev. C 60, 034614 (1999) [7 pages]

Strong absorption radii from reaction cross section measurements for neutron-rich nuclei

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N. Aissaoui1, N. Added1, N. Carlin1, G. M. Crawley2,3, S. Danczyk2, J. Finck4, M. M. de Moura1, D. Hirata5, D. J. Morrissey2,6, S. J. Sanders7, J. Stasko2, M. Steiner2, A. A. P. Suaide1, E. M. Szanto1, A. Szanto de Toledo1, M. Thoennessen2,3, and J. A. Winger8
1Departamento de Física Nuclear, Instituto de Física, Universidade de São Paulo, Caixa Postal 66318, 05315-970 São Paulo, São Paulo, Brazil
2National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824
3Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824
4Department of Physics, Central Michigan University, Mt. Pleasant, Michigan 48859
5Japan Synchrotron Radiation Research Institute (JASRI), Spring-8, Kamigori, Hyogo 678-12, Japan
6Department of Chemistry, Michigan State University, East Lansing, Michigan 48824
7Department of Physics and Astronomy, University of Kansas, Lawrence, Kansas 66045
8Department of Physics and Astronomy, Mississippi State University, Mississippi 39762

Received 23 March 1999; published 23 August 1999

Energy-integrated reaction cross sections have been measured at energies ranging from 38 to 80 MeV/nucleon for various exotic neutron-rich isotopes of Al, Si, P, S, Cl, Ar, K, Ca, Sc, and Ti stopping in Si. An experimental technique is employed where Si detectors are used for both particle identification and to serve as the target material. The reduced strong absorption radii r02 are deduced and compared with other experimental results. The radius dependence on the neutron number was studied and a trend of increasing reduced radius with neutron excess was found. This behavior is similar to that seen in lighter systems, although less pronounced than found there. The implications of this result on the conjectured existence of neutron halo or skin nuclei is discussed.

© 1999 The American Physical Society

URL:
http://link.aps.org/doi/10.1103/PhysRevC.60.034614
DOI:
10.1103/PhysRevC.60.034614
PACS:
25.60.Dz, 24.10.Ht, 27.30.+t, 27.40.+z
 
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