Past, Present and Future of the n_TOF Facility at CERN

Chiaveri, E.; Andriamonje, S.; Calviani, M.; Vlachoudis, V.; Brügger, M.; Cennini, P.; Cerutti, F.; Chin, M.; Ferrari, A.; Kadi, Y.; Lebbos, E.; Losito, R.; Guerrero, C.; Bécares, V.; Cano‐Ott, D.; Fernández‐Ordóñez, M.; González‐Romero, E.; Martı́nez, T.; Mendoza, E.; Ovejero, M. C.; Berthoumieux, E.; Gunsing, F.; Andrzejewski, J.; Marganiec, J.; Perkowski, J.; Audouin, L.; Berthier, B.; Tassan‐Got, L.; Bečvář, F.; Krtička, M.; Belloni, F.; Milazzo, Paolo; Calviño, F.; Hornillos, M. B. Gómez; Carrapiço, C.; Cortés, G.; Gonçalves, I. F.; Sarmento, R.; Vaz, P.; Colonna, N.; Marrone, S.; Meaze, M.; Tagliente, G.; Variale, V.; Cortés-Giraldo, M.A.; Lozano, M.; Praena, J.; Quesada, J.; Dillmann, I.; Domingo‐Pardo, C.; Heil, M.; Plag, R.; Reifarth, R.; Durán, I.; Paradela, C.; Tarrío, D.; Ganesan, S.; Giubrone, G.; Taín, J. L.; Gramegna, F.; Mastinu, P.; Harrisopulos, S.; Ioannides, K. G.; Karadimos, D.; Jericha, E.; Leeb, H.; Wei, Chuanshun; Käppeler, F.; Lederer, C.; Pavlik, A.; Wallner, A.; Massimi, C.; Vannini, G.; Mengoni, A.; Ventura, Alessandro; Mosconi, M.; Nolte, Roeland J. M.; Rubbia, C.; Vlastou, R.; Vykydal, Z.

doi:10.3938/jkps.59.1620

Cited by 6 publications

(10 citation statements)

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“…the DRAGON setup at TRIUMF (combined with recoil separator technique [7]) and LUNA at Gran Sasso [8] for charged particle induced reactions; and e.g. in Europe GELINA [9] and the n_TOF facility at CERN [10] for studying neutron-induced reactions.…”

Section: Andrpsdulvrq Ri µDfwlydwlrq $06 ¶ Zlwk Other Techniquesmentioning

confidence: 99%

Nuclear Data from AMS & Nuclear Data for AMS – some examples

Wallner

Bichler

Belgya

et al. 2012

EPJ Web of Conferences

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Abstract. We summarize some recent cross-section measurements using accelerator mass spectrometry (AMS). AMS represents an ultra-sensitive technique for measuring a limited, but steadily increasing number of longer-lived radionuclides. This method implies a two-step procedure with sample activation and subsequent AMS measurement. Applications include nuclear astrophysics, nuclear technology (nuclear fusion, nuclear fission and advanced reactor concepts and radiation dose estimations). A series of additional applications involves cosmogenic radionuclides in environmental, geological and extraterrestrial studies. There is a lack of information for a list of nuclides, as pointed out by nuclear data requests. An overview of some recent measurements is given and the method is illustrated for some specific neutron-induced reactions.

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Section: Andrpsdulvrq Ri µDfwlydwlrq $06 ¶ Zlwk Other Techniquesmentioning

confidence: 99%

Nuclear Data from AMS & Nuclear Data for AMS – some examples

Wallner

Bichler

Belgya

et al. 2012

EPJ Web of Conferences

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“…, M. Calviani 1) , V. Vlachoudis 1) , C. Weiß 2) , S. Andriamonje 1) , J. Andrzejewski 3) , L. Audouin 4) , V. Avrigeanu 5) , M. Barbagallo 6) , V. Bécares 7) , F. Bečvář 8) , F. Belloni 9) , E. Berthoumieux 1,9) , J. Billowes 10) , V. Boccone 1) , M. Brugger 1) , F. Calviño 11) , D. Cano-Ott 7) , C. Carrapiço 12) , F. Cerutti 1) , M. Chin 1) , N. Colonna 6) , G. Cortés 11) , M.A. Cortés-Giraldo 13) , M. Diakaki 14) , I. Dillmann 15) , C. Domingo-Pardo 16) , I. Duran 17) , N. Dzysiuk 18) , C. Eleftheriadis 19) , M. Fernández-Ordóñez 7) , A. Ferrari 1) , K. Fraval 9) , S. Ganesan 20) , G. Giubrone 21) , M.B.…”

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“…Cortés-Giraldo 13) , M. Diakaki 14) , I. Dillmann 15) , C. Domingo-Pardo 16) , I. Duran 17) , N. Dzysiuk 18) , C. Eleftheriadis 19) , M. Fernández-Ordóñez 7) , A. Ferrari 1) , K. Fraval 9) , S. Ganesan 20) , G. Giubrone 21) , M.B. Gómez-Hornillos 11) , I.F.…”

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“…Gonçalves 12) , E. González-Romero 7) , F. Gramegna 18) , E. Griesmayer 2) , C. Guerrero 1) , F. Gunsing 9) , M. Heil 16) , D.G. Jenkins 22) , E. Jericha 2) , Y. Kadi 1) , F. Käppeler 23) , D. Karadimos 24) , M. Kokkoris 14) , M. Krtička 8) , J. Kroll 8) , C. Lederer 25) , H. Leeb 2) , L.S. Leong 4) , R. Losito 1) , M. Lozano 13) , A. Manousos 19) , J. Marganiec 3) , T. Martinez 7) , C. Massimi 26) , P.F.…”

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“…Jenkins 22) , E. Jericha 2) , Y. Kadi 1) , F. Käppeler 23) , D. Karadimos 24) , M. Kokkoris 14) , M. Krtička 8) , J. Kroll 8) , C. Lederer 25) , H. Leeb 2) , L.S. Leong 4) , R. Losito 1) , M. Lozano 13) , A. Manousos 19) , J. Marganiec 3) , T. Martinez 7) , C. Massimi 26) , P.F. Mastinu 18) , M. Mastromarco 6) , M. Meaze 6) , E. Mendoza 7) , A. Mengoni 27) , P.M. Milazzo 28) , M. Mirea 5) , C. Paradela 17) , A. Pavlik 25) , J. Perkowski 3) , J. Praena 13) , J.M.…”

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Present status and future programs of the n_TOF experiment

Chiaveri

Calviani

Vlachoudis

et al. 2012

EPJ Web of Conferences

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Nuclear astrophysics with neutrons

Dillmann

Reifarth

2012

J. Inst.

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Neutrons play a crucial role in astrophysics during the heavy element nucleosynthesis. The largest fraction of isotopes heavier than iron is produced by neutron capture processes on short (r process) and long timescales (s process). During the "slow neutron capture process" (s process) heavier elements are produced by successive captures of in-situ produced neutrons from the reactions 13 C(α,n) 16 O and 22 Ne(α,n) 25 Mg (with densities of 10 6 − 10 10 cm −3 ) in the interior of stars and following β -decays. With this scenario the reaction path runs along the valley of stability up to 209 Bi and produces about 50% of the solar abundances of the heavy elements. Important nuclear physics parameters for s-process nucleosynthesis are neutron capture cross sections (for E n = 0.3-300 keV, corresponding to stellar temperatures between kT = 8 and 90 keV) and β -decay half-lives. Neutron capture measurements can be performed via activation in a quasi-stellar neutron spectrum utilizing several (p, n) reactions, or by the time-of-flight technique.The "rapid neutron capture process" (r process) is responsible for the remaining 50% of the solar abundances. Here neutrons with densities of 10 20 − 10 30 cm −3 are captured on a very fast timescale (ms) during a Core Collapse Supernova in a region close to the forming neutron star. The r-process nuclei are thus very short-lived, neutron-rich isotopes up to the actinides, which can only be produced and investigated at large-scale radioactive-beam facilities. Here the most important nuclear physics parameters are masses, half-lives, and at later stages also β -delayed neutrons. This paper will summarize the role of neutrons in nuclear astrophysics and give a short overview about the related astrophysics programs at the GSI Helmholtz research center and the FRANZ facility in Germany.

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Past, Present and Future of the n_TOF Facility at CERN

Cited by 6 publications

References 0 publications

Nuclear Data from AMS & Nuclear Data for AMS – some examples

Nuclear Data from AMS & Nuclear Data for AMS – some examples

Present status and future programs of the n_TOF experiment

Nuclear astrophysics with neutrons

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