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Spallation residues in the reaction ^(56)Fe + p at 0.3A, 0.5A, 0.75A, 1.0A, and 1.5A GeV

Villagrasa-Canton, C. and Boudard, A. and Ducret, J.-E. and Fernandez, B. and Leray, S. and Volant, C. and Armbruster, P. and Enqvist, T. and Hammache, F. and Helariutta, K. and Jurado, B. and Ricciardi, M.-V. and Schmidt, K.-H. and Sümmerer, K. and Vivès, F. and Yordanov, O. and Audouin, L. and Bacri, C.-O. and Ferrant, L. and Napolitani, P. and Rejmund, F. and Stéphan, C. and Tassan-Got, L. and Benlliure, J. and Casarejos, E. and Fernandez-Ordoñez, M. and Pereira, J. and Czajkowski, S. and Karamanis, D. and Pravikoff, M. and George, J. S. and Mewaldt, R. A. and Yanasak, N. and Wiedenbeck, M. and Connell, J. J. and Faestermann, T. and Heinz, A. and Junghans, A. (2007) Spallation residues in the reaction ^(56)Fe + p at 0.3A, 0.5A, 0.75A, 1.0A, and 1.5A GeV. Physical Review C, 75 (4). 044603. ISSN 0556-2813. doi:10.1103/PhysRevC.75.044603.

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The spallation residues produced in the bombardment of ^(56)Fe at 1.5A, 1.0A, 0.75A, 0.5A, and 0.3A GeV on a liquid-hydrogen target have been measured using the reverse kinematics technique and the fragment separator at GSI (Darmstadt). This technique has permitted the full identification in charge and mass of all isotopes produced with cross sections larger than 10^(-2) mb down to Z=8. Their individual production cross sections and recoil velocities at the five energies are presented. Production cross sections are compared with previously existing data and with empirical parametric formulas, often used in cosmic-ray astrophysics. The experimental data are also extensively compared with the results of different combinations of intranuclear cascade and deexcitation models. It is shown that the yields of the lightest isotopes cannot be accounted for by standard evaporation models. The GEMINI model, which includes an asymmetric fission decay mode, gives an overall good agreement with the data. These experimental data can be directly used for the estimation of composition modifications and damages in materials containing iron in spallation sources. They are also useful for improving high-precision cosmic-ray measurements.

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Mewaldt, R. A.0000-0003-2178-9111
Additional Information:© 2007 American Physical Society. Received 24 October 2006; published 13 April 2007. This experiment has benefited from a flexible and efficient operation of the GSI accelerators. Many thanks to all the operating team. The technical support of K. H. Behr, A. Brunle, and K. Burkard was crucial to the preparation of the experimental setup, and the liquid target was smoothly managed by P. Chesny, J.M. Gheller, and G. Guiller.We thank them all for their contributions. Comparison with irradiation experiments (Figs. 14 and 15) was possible thanks to the help of J. C. David and the kindness of Pr. R. Michel in providing us the experimental file. We thank also A. Botvina for helping us identify the multifragmentation contribution in the SMM code. During the interpretation of these results, we benefited greatly from fruitful discussions with J. Cugnon and Y. Yariv.
Group:Space Radiation Laboratory
Issue or Number:4
Classification Code:PACS number(s): 25.40.Sc, 25.70.Mn, 21.60.Ka
Record Number:CaltechAUTHORS:20091201-140054567
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Official Citation:Spallation residues in the reaction [sup 56]Fe + p at 0.3A,0.5A,0.75A,1.0A, and 1.5A GeV C. Villagrasa-Canton, A. Boudard, J.-E. Ducret, B. Fernandez, S. Leray, C. Volant, P. Armbruster, T. Enqvist, F. Hammache, K. Helariutta, B. Jurado, M.-V. Ricciardi, K.-H. Schmidt, K. Summerer, F. Vives, O. Yordanov, L. Audouin, C.-O. Bacri, L. Ferrant, P. Napolitani, F. Rejmund, C. Stephan, L. Tassan-Got, J. Benlliure, E. Casarejos, M. Fernandez-Ordonez, J. Pereira, S. Czajkowski, D. Karamanis, M. Pravikoff, J. S. George, R. A. Mewaldt, N. Yanasak, M. Wiedenbeck, J. J. Connell, T. Faestermann, A. Heinz, and A. Junghans, Phys. Rev. C 75, 044603 (2007), DOI:10.1103/PhysRevC.75.044603
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:16850
Deposited On:03 Dec 2009 22:13
Last Modified:08 Nov 2021 23:30

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