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1. Investigation of a light Dark Boson existence: The New JEDI project

Author

Beyhan Bastin, Jürgen Kiener, Isabelle Deloncle, Alain Coc, Maxim Pospelov, Jaromir Mrazek, Livio Lamia, Dieter Ackermann, Philip Adsley, Charles-Olivier Bacri, Jérôme Bourçois, Vaclav Burjan, Anastasia Cassisa, Giuseppe D’agata, Gilles De France, Alessia Di Pietrio, Yasmine Demane, François De Oliveira, Lindsay Donaldson, Corinne Donzaud, Jean-Eric Ducret, Clarisse Hamadache, Fairouz Hammache, Pete Jones, Marco La Cognata, Adrien Laviron, Marek Lewitowicz, Kgashane Malatji, Antonio Massara, Cyril Pitrou, Rosario Gianluca Pizzone, Giovanni Luca Guardo, Marek Płoszajczak, Giuseppe Rapisarda, Bernadette Rebeiro, Brigitte Roussèire, Domenico Santonocito, Nicolas de Séréville, Maria Letizia Sergi, Eva Simeckova, Olivier Sorlin, Christelle Stodel, Vincent Tatischeff, Jean-Charles Thomas, Aurora Tumino, Grand Accélérateur National d'Ions Lourds (GANIL), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
messenger, star, gas, anomaly, hidden sector, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], new particle
Abstract

Several experiments around the world are looking for a new particle, named Dark Boson, which may do the link between the Ordinary Matter (which forms basically stars, planets, interstellar gas...) and the Hidden Sectors of the Universe. This particle, if it exists, would act as the messenger of a new fundamental interaction of nature. In this paper, the underlying Dark Sectors theory will be introduced first. A non-exhaustive summary of experimental studies carried out to date and foreseen in the incoming years will be presented after,including the 8Be anomaly. The last section will provide a status of the New JEDI**** project which aims to investigate the existence or not of a Dark Boson in the MeV range.

Published
2022
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2. γ -ray emission in α -particle interactions with C, Mg, Si, and Fe at Eα=50–90 MeV

Author

H. Benhabiles, C. Hamadache, I. Deloncle, A. Gostojic, R. Mezhoud, I. Bourgaoub, Andrea Denker, Fairouz Hammache, Vincent Tatischeff, Jürgen Bundesmann, Jörg Röhrich, Jürgen Kiener, J. Peyré, and A. Coc

Subjects
Nuclear reaction, Physics, Solar flare, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Center (category theory), 7. Clean energy, 01 natural sciences, Base (group theory), Excited state, 0103 physical sciences, Production (computer science), Emission spectrum, Atomic physics, Nuclear Experiment, 010306 general physics, Energy (signal processing)
Abstract

Nuclear deexcitation lines are regularly observed in the $\ensuremath{\gamma}$-ray emission spectra of strong solar flares. The most prominent lines are produced by interactions of protons and $\ensuremath{\alpha}$ particles, accelerated up to hundreds of MeV, with abundant nuclei of the solar atmosphere. Analysis and interpretation of these lines, which carry valuable information on the solar flare properties, need cross-section data for the $\ensuremath{\gamma}$-ray line emission in these interactions for a wide particle energy range. To this purpose, we measured the $\ensuremath{\gamma}$-ray emission in interactions of $\ensuremath{\alpha}$-particle beams of ${E}_{\ensuremath{\alpha}}=50\text{--}90$ MeV with target foils of C, Mg, Si, and Fe at the center for proton therapy of the Helmholtz-Zentrum Berlin. Setups of three high-purity Ge detectors and one $\mathrm{La}{\mathrm{Br}}_{3}$:Ce detector have been employed to detect the $\ensuremath{\gamma}$ rays in two experiment campaigns. Relatively large distances of the detectors from the target and pulsed beams with sub-ns-wide pulses allowed the separation of beam-induced prompt $\ensuremath{\gamma}$-ray emission from the targets from other $\ensuremath{\gamma}$ rays and neutron-induced background. $\ensuremath{\gamma}$-ray production cross sections for about 60 deexcitation lines from excited target nuclei or reaction products have been determined. For the strongest deexcitation lines from the major target isotopes, $^{12}\mathrm{C}$, $^{24}\mathrm{Mg}$, $^{28}\mathrm{Si}$, $^{56}\mathrm{Fe}$, there are now measured cross-section data from reaction threshold to ${E}_{\ensuremath{\alpha}}=90$ MeV that can be directly used for astrophysical applications like solar flares. Comparison of the results with a cross-section compilation for strong $\ensuremath{\gamma}$-ray lines in solar flare emissions and the predictions of the talys nuclear reaction code were done. They underline the importance of cross-section determinations at accelerator laboratories for the establishment of an accurate cross-section data base in a wide projectile energy range.

Published
2021
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3. Optimization of CeBr$_3$ position-sensitive calorimeter module

Author

Clarisse Hamadache, Adrien Laviron, V. Tatischeff, Jean Peyré, Corentin Hiver, Valentin Gourlaouen, Jürgen Kiener, Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), and Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)

Subjects
Artificial neural network, Nuclear and High Energy Physics, Test bench, Physics::Instrumentation and Detectors, Photodetector, Scintillator, 01 natural sciences, Collimated light, Optics, Position reconstruction, Position (vector), gamma-ray astronomy, 0103 physical sciences, Compton imaging, 010303 astronomy & astrophysics, Instrumentation, Physics, [PHYS]Physics [physics], Spatial resolution, 010308 nuclear & particles physics, business.industry, Detector, Scintillating calorimeter, Calorimeter, Theano, Cerium bromide, business
Abstract

International audience; For the next generation of MeV range gamma-ray telescopes, position sensitive calorimeters based on a monolithic scintillator coupled to a pixelated photodetector could be an important building block. In this paper, we present the optimization of the position reconstruction algorithms using machine learning, for a detector based on a 51×51×10mm3 CeBr 3 crystal. For that purpose, we used an automated test bench and collimated radioactive sources to generate experimental data of known energy and position by irradiating the detector with gamma rays. We found in these data different gamma-ray interaction morphologies for which position reconstruction algorithms perform differently, and we developed an algorithm to automatically classify them. We also conducted an extensive optimization of the artificial neural networks that perform the 3D position reconstruction using the Keras Python library with Theano backend. We found that at 662keV , 90% of events have a morphology that facilitates position reconstruction. The optimized position reconstruction algorithms give for those events a rms error in the plane of the detector of 1.8mm on each axis. The rms error in the depth of the crystal is found to be 2mm .

Published
2021
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4. Evaluation of the N13(α,p)O16 thermonuclear reaction rate and its impact on the isotopic composition of supernova grains

Author

D. Beaumel, Fairouz Hammache, L. Audouin, M. G. Pellegriti, Marco Pignatari, Richard Longland, T. Lawson, S. Fortier, Vincent Tatischeff, A. Lefebvre-Schuhl, Anne Meyer, Alison Laird, N. de Séréville, Jürgen Kiener, and M. Stanoiu

Subjects
Physics, 010308 nuclear & particles physics, Monte Carlo method, chemistry.chemical_element, Context (language use), 7. Clean energy, 01 natural sciences, Reaction rate, Nuclear physics, Supernova, Stars, chemistry, 13. Climate action, 0103 physical sciences, Born approximation, 010306 general physics, Stellar evolution, Helium
Abstract

Background: It has been recently suggested that hydrogen ingestion into the helium shell of massive stars could lead to high C13 and N15 excesses when the shock of a core-collapse supernova passes through its helium shell. This prediction questions the origin of extremely high C13 and N15 abundances observed in rare presolar SiC grains which is usually attributed to classical novae. In this context the N13(α,p)O16 reaction plays an important role since it is in competition with N13β+ decay to C13. Purpose: The N13(α,p)O16 reaction rate used in stellar evolution calculations comes from the Caughlan and Fowler compilation with very scarce information on the origin of this rate and with no associated uncertainty. The goal of this work is to provide a recommended N13(α,p)O16 reaction rate, based on available experimental data, with a meaningful statistical uncertainty. Method: Unbound nuclear states in the F17 compound nucleus were studied using the spectroscopic information of the analog states in O17 nucleus that were measured at the Tandem-Alto facility using the C13(Li7,t)O17 α-particle-transfer reaction. The α-particle spectroscopic factors were derived using a finite-range distorted-wave Born approximation analysis. This spectroscopic information was used to calculate a recommended N13(α,p)O16 reaction rate with meaningful uncertainty using a Monte Carlo approach. Results: The N13(α,p)O16 reaction rate from the present work is found to be within a factor of two of the previous evaluation in the temperature range of interest, with a typical uncertainty of a factor ≈2-3. The source of this uncertainty has been identified to come from the three main contributing resonances at Erc.m.=221, 741, and 959 keV. This new error estimation translates to an overall uncertainty in the C13 production of a factor of 50 when using the lower and upper reaction rates in the conditions relevant for the N13(α,p)O16 activation. Conclusions: The main source of uncertainty on the re-evaluated N13(α,p)O16 reaction rate currently comes from the uncertain α-particle width of relevant F17 states.

Published
2020
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5. Charged-particle decays of highly excited states in $^{19}$F

Author

I. Stefan, I. Sivacek, Marin Chabot, Jérôme Guillot, A. Gottardo, M. Assié, C. Delafosse, A. Georgiadou, J. Riley, Vincent Tatischeff, L. Perrot, Alison Laird, D. Beaumel, I. Matea, F. Flavigny, Valdir Guimaraes, P. Adsley, Jürgen Kiener, S. P. Fox, R. Garg, M. Degerlier, A. Lefebvre-Schuhl, N. de Sereville, L. Olivier, S. Gillespie, Fairouz Hammache, Institut de Physique Nucléaire d'Orsay (IPNO), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), and Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)

Subjects
Physics, 010308 nuclear & particles physics, Order (ring theory), FOS: Physical sciences, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], 01 natural sciences, Charged particle, Supernova, Excited state, 0103 physical sciences, Production (computer science), Neutron, Atomic physics, Nuclear Experiment (nucl-ex), Nuclear Experiment, 010303 astronomy & astrophysics
Abstract

Neutron-capture reactions on $^{18}$F in the helium-burning shell play an important role in the production of $^{15}$N during core-collapse supernovae. The competition between the $^{18}$F($n,p/\alpha$)$^{18}$O/$^{15}$N reactions controls the amount of $^{15}$N produced. The strengths of these reactions depend on the decay branching ratios of states in $^{19}$F above the neutron threshold. We report on an experiment investigating the decay branching ratios of these states in order to better constrain the strengths of the reactions., Comment: Submitted as part of the Proceedings of NIC 2018

Published
2018
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6. Exploring the Capabilities of the Anti-Coincidence Shield of the International Gamma-Ray Astrophysics Laboratory (INTEGRAL) Spectrometer to Study Solar Flares

Author

Jürgen Kiener, Karl-Ludwig Klein, Nicole Vilmer, C. Hamadache, Rosa Rodríguez-Gasén, Vincent Tatischeff, CSNSM AN, Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)-Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), and Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)

Subjects
[PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Photon, 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Highly elliptical orbit, Instrumental effects, Astrophysics, 01 natural sciences, 7. Clean energy, symbols.namesake, Observatory, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Spectrometer, Spacecraft, Solar flare, Flares, business.industry, association with flares, Astronomy and Astrophysics, energetic particles, Orbital period, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 13. Climate action, Space and Planetary Science, Van Allen radiation belt, Physics::Space Physics, X-ray bursts, symbols, Astrophysics::Earth and Planetary Astrophysics, business
Abstract

The International Gamma-Ray Astrophysics Laboratory (INTEGRAL) is a European Space Agency hard X-ray/γ-ray observatory for astrophysics, covering photon energies from 15 keV to 10 MeV. It was launched in 2002, and since then the Bismuth Germanate (BGO) detectors of the Anti-Coincidence Shield (ACS) of the Spectrometer on INTEGRAL (SPI) have detected many hard X-ray (HXR) bursts from the Sun, producing light curves at photon energies above ≈ 100 keV. The spacecraft has a highly elliptical orbit, providing long uninterrupted observing (about 90 % of the orbital period) with nearly constant background due to the shorter time needed to cross Earth's radiation belts. However, because of technical constraints, INTEGRAL cannot be pointed at the Sun, and high-energy solar photons are always detected in nonstandard observation conditions. To make the data useable for solar studies, we have undertaken a major effort to specify the observing conditions through Monte Carlo simulations of the response of ACS for several selected flares. We checked the performance of the model employed for the Monte Carlo simulations using the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) observations for the same sample of solar flares. We conclude that although INTEGRAL was not designed to perform solar observations, ACS is a useful instrument for solar-flare research. In particular, its relatively large effective area allows determining good-quality HXR/γ-ray light curves for X- and M-class solar flares and, in some cases, probably also for C-class flares.

Published
2013
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7. An above-barrier narrow resonance in F-15

Author

F. de Grancey, M. Fadil, Marek Ploszajczak, Nicolas Michel, N. A. Smirnova, I. Stefan, M. Assié, F. de Oliveira Santos, V. Chudoba, J. M. Daugas, R. Borcea, J. C. Thomas, E. Berthoumieux, J. C. Angélique, Thomas Davinson, O. Roig, Predrag Ujić, Igor T. Čeliković, L. Perrot, F. Negoita, A. Mercenne, F. Rotaru, M. G. Pellegriti, C. Stodel, G. Dumitru, G. Randisi, M. G. Saint Laurent, I. Ray, A. Lefebvre-Schuhl, R. Wolski, S. Grévy, A. Buta, O. Sorlin, J. Okolowicz, Vincent Tatischeff, J. Mrazek, M. Stanoiu, Jürgen Kiener, D. Pantelica, K. Subotic, Grand Accélérateur National d'Ions Lourds (GANIL), Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire de physique corpusculaire de Caen (LPCC), Université de Caen Normandie (UNICAEN), Normandie Université (NU)-Normandie Université (NU)-École Nationale Supérieure d'Ingénieurs de Caen (ENSICAEN), Normandie Université (NU)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut de Physique Nucléaire d'Orsay (IPNO), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Direction des Applications Militaires (DAM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Normandie Université (NU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Nuclear and High Energy Physics, Proton, Nuclear Theory, FOS: Physical sciences, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], Elastic proton scattering, lifetimes, width, 01 natural sciences, Unbound States, 0103 physical sciences, Unbound states, medicine, Neutron, Nuclear Experiment (nucl-ex), 010306 general physics, Wave function, Nuclear Experiment, 15F, Elastic scattering, Physics, Valence (chemistry), 25.60.-t, 25.70.Ef, 25.40.Cm, 21.10.-k, 27.20.+n, 21.10.Tg, 010308 nuclear & particles physics, F-15, Resonance, Overbarrier resonance, lcsh:QC1-999, width, medicine.anatomical_structure, Excited state, Resonances, lifetimes, Physics::Accelerator Physics, Atomic physics, Elastic proton scattering, Nucleus, lcsh:Physics
Abstract

Intense and purified radioactive beam of post-accelerated $^{14}$O was used to study the low-lying states in the unbound $^{15}$F nucleus. Exploiting resonant elastic scattering in inverse kinematics with a thick target, the second excited state, a resonance at E$\_R$=4.757(6)(10)~MeV with a width of $\Gamma$=36(5)(14)~keV was measured for the first time with high precision. The structure of this narrow above-barrier state in a nucleus located two neutrons beyond the proton drip line was investigated using the Gamow Shell Model in the coupled channel representation with a $^{12}$C core and three valence protons. It is found that it is an almost pure wave function of two quasi-bound protons in the $2s\_{1/2}$ shell., Comment: 8 pages, 2 figures, 1 table, Submitted to Phys. Lett. B

Published
2016
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8. Study of the 26 Al(n,p) 26 Mg and 26 Al(n,α) 23 Na reactions using the 27 Al(p,p') 27 Al inelastic scattering reaction

Author

I. Deloncle, G. Mavilla, B. Le Crom, Fairouz Hammache, C. T. Nsangu, P. Roussel, P. Adsley, Alison Laird, Marine Vandebrouck, S. Ancelin, Vincent Tatischeff, J. Guillot, S. P. Fox, C. Hamadache, I. Stefan, N. Oulebsir, M. Assié, C. J. Barton, L. Perrot, G. Marquinez Duran, S. Benamara, D. Suzuki, P. Morfouace, L. Lefebvre, C. A. Diget, N. de Séréville, Jürgen Kiener, A. Lefebfre-Schuhl, A. Coc, A. M. Sánchez-Benítez, and A. Mutschler

Subjects
Nuclear reaction, Physics, History, 010504 meteorology & atmospheric sciences, Isotope, Radiochemistry, Inelastic scattering, 010502 geochemistry & geophysics, Isotopes of sodium, 01 natural sciences, Computer Science Applications, Education, Nucleosynthesis, Neutron, Alpha decay, Isotopes of magnesium, 0105 earth and related environmental sciences
Abstract

26Al was the first cosmic radioactivity ever detected in the galaxy as well as one of the first extinct radioactivity observed in refractory phases of meteorites. Its nucleosynthesis in massive stars is still uncertain mainly due to the lack of nuclear information concerning the 26Al(n,p)26Mg and 26Al(n,α)23Na reactions. We report on a single and coincidence measurement of the 27Al(p,p’)27Al(p)26Mg and 27Al(p,p’)27Al(α)23Na reactions performed at the Orsay TANDEM facility aiming at the spectroscopy study of 27Al above the neutron threshold. Fourteen states are observed for the first time within 350 keV above the 26Al+n threshold.

Published
2016

9. Indirect study of 19Ne states near the threshold

Author

N. de Séréville, B. Bouzid, Marc Loiselet, Jürgen Kiener, Carmen Angulo, Vincent Tatischeff, A. Coc, Michel Gaelens, P. Figuera, F. de Oliveira Santos, Guido Ryckewaert, Daniel Labar, Alain Ninane, S. Fortier, S. Ouichaoui, P. Demaret, Marlete Assunção, S. Cherubini, F. Hammache, Pierre Leleux, E. Berthoumieux, D. Beaumel, N. Smirnova, Manoel Couder, and A. Lefebvre-Schuhl

Subjects
Physics, Reaction rate, Nuclear reaction, Nuclear and High Energy Physics, Proton, 010308 nuclear & particles physics, Scattering, 0103 physical sciences, Atomic physics, 010306 general physics, 01 natural sciences, Radioactive beam
Abstract

The early E ⩽ 511 keV gamma-ray emission from novae depends critically on the F 18 ( p , α ) O 15 reaction. Unfortunately the reaction rate of the F 18 ( p , α ) O 15 reaction is still largely uncertain due to the unknown strengths of low-lying proton resonances near the F 18 + p threshold which play an important role in the nova temperature regime. We report here our last results concerning the study of the d ( F 18 , p ) F 19 ( α ) N 15 transfer reaction. We show in particular that these two low-lying resonances cannot be neglected. These results are then used to perform a careful study of the remaining uncertainties associated to the F 18 ( p , α ) O 15 and F 18 ( p , γ ) Ne 19 reaction rates.

Published
2007
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10. Spectroscopy ofNe19for the thermonuclearO15(α,γ)Ne19andF18(p,α)O15reaction rates

Author

Jürgen Kiener, N. de Séréville, Ralf Hertenberger, P. Adsley, Kathrin Wimmer, Fairouz Hammache, I. Stefan, H.-F. Wirth, B. R. Fulton, Anuj Parikh, Thomas Faestermann, D. Seiler, and Alison Laird

Subjects
Reaction rate, Physics, Nuclear and High Energy Physics, Thermonuclear fusion, Proton, Nuclear structure, Atomic physics, Type (model theory), Spectroscopy
Abstract

Uncertainties in the thermonuclear rates of the $^{15}\text{O}(\ensuremath{\alpha},\ensuremath{\gamma}){}^{19}\text{Ne}$ and ${}^{18}\text{F}(p,\ensuremath{\alpha}){}^{15}\text{O}$ reactions affect model predictions of light curves from type I x-ray bursts and the amount of the observable radioisotope $^{18}\text{F}$ produced in classical novae, respectively. To address these uncertainties, we have studied the nuclear structure of $^{19}\text{Ne}$ over ${E}_{x}=4.0\ensuremath{-}5.1$ and 6.1--7.3 MeV using the $^{19}\text{F}(^{3}\text{He},t)^{19}\text{Ne}$ reaction. We find the ${J}^{\ensuremath{\pi}}$ values of the 4.14- and 4.20-MeV levels to be consistent with $9/{2}^{\ensuremath{-}}$ and $7/{2}^{\ensuremath{-}}$, respectively, in contrast to previous assumptions. We confirm the recently observed triplet of states around 6.4 MeV and find evidence that the state at 6.29 MeV, just below the proton threshold, is either broad or a doublet. Our data also suggest that predicted but yet unobserved levels may exist near the 6.86-MeV state. Higher resolution experiments are urgently needed to further clarify the structure of $^{19}\text{Ne}$ around the proton threshold before a reliable ${}^{18}\text{F}(p,\ensuremath{\alpha}){}^{15}\text{O}$ rate for nova models can be determined.

Published
2015
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11. Recent results in nuclear astrophysics

Author

A. Coc, Fairouz Hammache, Jürgen Kiener, CSNSM AN, Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut de Physique Nucléaire d'Orsay (IPNO), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), and Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM)

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), [PHYS]Physics [physics], Physics, Nuclear and High Energy Physics, Astrophysics::High Energy Astrophysical Phenomena, Physics beyond the Standard Model, FOS: Physical sciences, Cosmic ray, Astrophysics, 7. Clean energy, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Stars, 13. Climate action, Nucleosynthesis, Nuclear astrophysics, Neutron source, Nuclear Experiment (nucl-ex), Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Energy source, Nuclear Experiment, Stellar evolution
Abstract

In this review, we emphasize the interplay between astrophysical observations, modeling, and nuclear physics laboratory experiments. Several important nuclear cross sections for astrophysics have long been identified e.g. 12C(alpha,gamma)16O for stellar evolution, or 13C(alpha,n)16O and 22Ne(alpha,n)25Mg as neutron sources for the s-process. More recently, observations of lithium abundances in the oldest stars, or of nuclear gamma-ray lines from space, have required new laboratory experiments. New evaluation of thermonuclear reaction rates now includes the associated rate uncertainties that are used in astrophysical models to i) estimate final uncertainties on nucleosynthesis yields and ii) identify those reactions that require further experimental investigation. Sometimes direct cross section measurements are possible, but more generally the use of indirect methods is compulsory in view of the very low cross sections. Non-thermal processes are often overlooked but are also important for nuclear astrophysics, e.g. in gamma-ray emission from solar flares or in the interaction of cosmic rays with matter, and also motivate laboratory experiments. Finally, we show that beyond the historical motivations of nuclear astrophysics, understanding i) the energy sources that drive stellar evolution and ii) the origin of the elements can also be used to give new insights into physics beyond the standard model., 38 pages, 33 Figures, invited review

Published
2015
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12. Fast-neutron induced background in LaBr3:Ce detectors

Author

M. S. Yavahchova, C. Blondel, G. Prévot, C. Hamadache, B. Horeau, N. de Séréville, I. Deloncle, A. Gostojic, O. Limousin, R. Rodríguez-Gasén, N. Goutev, Marin Chabot, P. Laurent, Fairouz Hammache, Jürgen Kiener, Vincent Tatischeff, Remi Chipaux, S. Dubos, A. Coc, S. Ouichaoui, CSNSM AN, Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)-Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), CSNSM SNO, Institut de Physique Nucléaire d'Orsay (IPNO), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Département d'Electronique, des Détecteurs et d'Informatique pour la Physique (ex SEDI) (DEDIP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, and Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM)

Subjects
Nuclear and High Energy Physics, Physics - Instrumentation and Detectors, Proton, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, Nuclear Theory, FOS: Physical sciences, Monte-Carlo simulation, Scintillator, 7. Clean energy, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Nuclear physics, NE-213, 0103 physical sciences, Neutron detection, Neutron, Irradiation, Nuclear Experiment (nucl-ex), Nuclear Experiment, 010303 astronomy & astrophysics, Instrumentation, Instrumentation and Methods for Astrophysics (astro-ph.IM), Neutron irradiation, [PHYS]Physics [physics], Bonner sphere, Physics, Range (particle radiation), 010308 nuclear & particles physics, Detector, Instrumentation and Detectors (physics.ins-det), LaBr3:Ce, HP-Ge, High Energy Physics::Experiment, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The response of a scintillation detector with a cylindrical 1.5-inch LaBr3:Ce crystal to incident neutrons has been measured in the energy range En = 2-12 MeV. Neutrons were produced by proton irradiation of a Li target at Ep = 5-14.6 MeV with pulsed proton beams. Using the time-of-flight information between target and detector, energy spectra of the LaBr3:Ce detector resulting from fast neutron interactions have been obtained at 4 different neutron energies. Neutron-induced gamma rays emitted by the LaBr3:Ce crystal were also measured in a nearby Ge detector at the lowest proton beam energy. In addition, we obtained data for neutron irradiation of a large-volume high-purity Ge detector and of a NE-213 liquid scintillator detector, both serving as monitor detectors in the experiment. Monte-Carlo type simulations for neutron interactions in the liquid scintillator, the Ge and LaBr3:Ce crystals have been performed and compared with measured data. Good agreement being obtained with the data, we present the results of simulations to predict the response of LaBr3:Ce detectors for a range of crystal sizes to neutron irradiation in the energy range En = 0.5-10 MeV, Comment: 28 pages, 10 figures, 4 Tables

Published
2015
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13. Probing nuclear forces beyond the drip-line using the mirror nuclei N16 and F16

Author

M. Lenhardt, Thomas Davinson, Vincent Tatischeff, I. Stefan, S. Grévy, F. de Grancey, J. C. Thomas, Marek Ploszajczak, J. Mrazek, M. Stanoiu, R. Borcea, C. Stodel, J. C. Angelique, M. G. Pellegriti, M. G. Saint Laurent, I. Ray, O. Roig, M. Lewitowicz, F. de Oliveira Santos, J. M. Daugas, M. Fadil, G. Dumitru, M. Angélique, Jürgen Kiener, A. Lefebvre-Schuhl, C. Borcea, A. Buta, D. Pantelica, F. Negoita, L. Perrot, E. Berthoumieux, and O. Sorlin

Subjects
Elastic scattering, Physics, Nuclear and High Energy Physics, Nuclear Theory, Nuclear force, Neutron, Symmetry breaking, Mirror nuclei, Atomic physics, Nuclear Experiment
Abstract

Radioactive beams of $^{14}\mathrm{O}$ and $^{15}\mathrm{O}$ were used to populate the resonant states ${1/2}^{+}$, ${5/2}^{+}$ and ${0}^{\ensuremath{-}},{1}^{\ensuremath{-}},{2}^{\ensuremath{-}}$ in the unbound $^{15}\mathrm{F}$ and $^{16}\mathrm{F}$ nuclei, respectively, by means of proton elastic scattering reactions in inverse kinematics. Based on their large proton spectroscopic factor values, the resonant states in $^{16}\mathrm{F}$ can be viewed as a core of $^{14}\mathrm{O}$ plus a proton in the $2{s}_{1/2}$ or $1{d}_{5/2}$ shell and a neutron in $1{p}_{1/2}$. Experimental energies were used to derive the strength of the $2{s}_{1/2}$-$1{p}_{1/2}$ and $1{d}_{5/2}$-$1{p}_{1/2}$ proton-neutron interactions. It is found that the former changes by 40% compared with the mirror nucleus $^{16}\mathrm{N}$, and the latter changes by 10%. This apparent symmetry breaking of the nuclear force between mirror nuclei finds explanation in the role of the large coupling to the continuum for the states built on an $\ensuremath{\ell}=0$ proton configuration.

Published
2014
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16. The first SEPServer event catalogue ~68-MeV solar proton events observed at 1 AU in 1996–2010

Author

Rami Vainio, Eino Valtonen, Bernd Heber, Olga E. Malandraki, Athanasios Papaioannou, Karl‐Ludwig Klein, Alexander Afanasiev, Neus Agueda, Henry Aurass, Markus Battarbee, Stephan Braune, Wolfgang Dröge, Urs Ganse, Clarisse Hamadache, Daniel Heynderickx, Kalle Huttunen-Heikinmaa, Jürgen Kiener, Patrick Kilian, Andreas Kopp, Athanasios Kouloumvakos, Sami Maisala, Alexander Mishev, Rositsa Miteva, Alexander Nindos, Tero Oittinen, Osku Raukunen, Esa Riihonen, Rosa Rodríguez-Gasén, Oskari Saloniemi, Blai Sanahuja, Renate Scherer, Felix Spanier, Vincent Tatischeff, Kostas Tziotziou, Ilya G. Usoskin, Nicole Vilmer, and Universitat de Barcelona

Subjects
Atmospheric Science, Radiació solar, 010504 meteorology & atmospheric sciences, Proton, Meteorology, Solar cycle 23, Astrophysics, lcsh:QC851-999, Space weather, Electromagnetisme, 7. Clean energy, 01 natural sciences, Partícules (Física nuclear), law.invention, Electromagnetism, Path length, law, 0103 physical sciences, Solar radiation, Astrophysics::Solar and Stellar Astrophysics, media_common.cataloged_instance, European union, 010303 astronomy & astrophysics, Particles (Nuclear physics), 0105 earth and related environmental sciences, media_common, Physics, ta115, Sol, Sun, projects, radio emissions (dynamic), flares, radiation, Particle acceleration, SEP, 13. Climate action, Space and Planetary Science, Physics::Space Physics, lcsh:Meteorology. Climatology, Heliosphere, Flare
Abstract

SEPServer is a three-year collaborative project funded by the seventh framework programme (FP7-SPACE) of the European Union. The objective of the project is to provide access to state-of-the-art observations and analysis tools for the scientific community on solar energetic particle (SEP) events and related electromagnetic (EM) emissions. The project will eventually lead to better understanding of the particle acceleration and transport processes at the Sun and in the inner heliosphere. These processes lead to SEP events that form one of the key elements of space weather. In this paper we present the first results from the systematic analysis work performed on the following datasets: SOHO/ERNE, SOHO/EPHIN, ACE/EPAM, Wind/WAVES and GOES X-rays. A catalogue of SEP events at 1 AU, with complete coverage over solar cycle 23, based on high-energy (~68-MeV) protons from SOHO/ERNE and electron recordings of the events by SOHO/EPHIN and ACE/EPAM are presented. A total of 115 energetic particle events have been identified and analysed using velocity dispersion analysis (VDA) for protons and time-shifting analysis (TSA) for electrons and protons in order to infer the SEP release times at the Sun. EM observations during the times of the SEP event onset have been gathered and compared to the release time estimates of particles. Data from those events that occurred during the European day-time, i.e., those that also have observations from ground-based observatories included in SEPServer, are listed and a preliminary analysis of their associations is presented. We find that VDA results for protons can be a useful tool for the analysis of proton release times, but if the derived proton path length is out of a range of 1 AU

Published
2013
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17. Search for superscreening effects in a superconductor

Author

F. de Oliveira Santos, B. Bastin, M. G. Saint Laurent, Vincent Tatischeff, R. Borcea, M. Lewitowicz, A. Buta, A. Coc, C. Borcea, Predrag Ujić, M. Stanoiu, A. Lepailleur, N. L. Achouri, O. Sorlin, Jürgen Kiener, Alain Pautrat, O. Kamalou, M. Assié, V. Méot, Grand Accélérateur National d'Ions Lourds (GANIL), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Vinča Institute of Nuclear Sciences, University of Belgrade [Belgrade], Laboratoire de physique corpusculaire de Caen (LPCC), Université de Caen Normandie (UNICAEN), Normandie Université (NU)-Normandie Université (NU)-École Nationale Supérieure d'Ingénieurs de Caen (ENSICAEN), Normandie Université (NU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire d'Orsay (IPNO), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Horia Hulubei National Institute of Physics and Nuclear Engineering (NIPNE), IFIN-HH, CSNSM AN, Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), DAM Île-de-France (DAM/DIF), Direction des Applications Militaires (DAM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire de cristallographie et sciences des matériaux (CRISMAT), Normandie Université (NU)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche sur les Matériaux Avancés (IRMA), Normandie Université (NU)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université de Rouen Normandie (UNIROUEN), Normandie Université (NU)-Institut national des sciences appliquées Rouen Normandie (INSA Rouen Normandie), Institut National des Sciences Appliquées (INSA)-Normandie Université (NU)-Institut National des Sciences Appliquées (INSA)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université de Rouen Normandie (UNIROUEN), Institut National des Sciences Appliquées (INSA)-Normandie Université (NU)-Institut National des Sciences Appliquées (INSA)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Normandie Université (NU)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)-Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), École Nationale Supérieure d'Ingénieurs de Caen (ENSICAEN), Normandie Université (NU)-Normandie Université (NU)-Centre National de la Recherche Scientifique (CNRS)-Université de Caen Normandie (UNICAEN), and Normandie Université (NU)-Institut de Chimie du CNRS (INC)

Subjects
Niobium, FOS: Physical sciences, General Physics and Astronomy, chemistry.chemical_element, Lifetimes, Beta decay, Electron, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], 01 natural sciences, Hydrostatic stellar nucleosynthesis, Widths, Double beta decay, Error bar, 0103 physical sciences, 23.40.-s, 21.10.Tg, 27.20.+n, 74.25.-q, Nuclear Experiment (nucl-ex), 010306 general physics, Nuclear Experiment, Physics, Superconductivity, 010308 nuclear & particles physics, Properties of superconductors, Potential energy, 3. Good health, chemistry, Atomic physics, 6 < A < 19
Abstract

The decay of $^{19}$O($\beta^-$) and $^{19}$Ne($\beta^+$) implanted in niobium in its superconducting and metallic phase was measured using purified radioactive beams produced by the SPIRAL/GANIL facility. Half-lives and branching ratios measured in the two phases are consistent within one-sigma error bar. This measurement casts strong doubts on the predicted strong electron screening in superconductor, the so-called superscreening. The measured difference in screening potential energy is 110(90) eV for $^{19}$Ne and 400(320) eV for $^{19}$O. Precise determinations of the half-lives were obtained for $^{19}$O: 26.476(9) s and $^{19}$Ne: 17.254(5) s., Comment: 4 pages, 3 figures, accepted for publication in Physical Review Letters

Published
2012
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18. Spectroscopy of $^{18}$Na: Bridging the two-proton radioactivity of $^{19}$Mg

Author

F. de Oliveira Santos, A. Lefebvre-Schuhl, T. Al Kalanee, C. Borcea, L. Perrot, R. Wolski, K. Subotic, J. C. Angélique, A. M. Sánchez-Benítez, F. Rotaru, Y. H. Lam, T. Davinson, R. Borcea, Predrag Ujić, V. Chudoba, Muriel Fallot, M. Stanoiu, L. Caceres, J. Mrazek, M. Assié, Igor T. Čeliković, Gavin Lotay, F. de Grancey, L. Achouri, C. Ducoin, O. Kamalou, Yu. Sobolev, P. J. Woods, Jürgen Kiener, J. Alcantara-Nunez, M. G. Saint-Laurent, NA Smirnova, D.Y. Pang, I. Stefan, Grand Accélérateur National d'Ions Lourds (GANIL), Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut de Physique Nucléaire d'Orsay (IPNO), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Laboratoire de physique corpusculaire de Caen (LPCC), Université de Caen Normandie (UNICAEN), Normandie Université (NU)-Normandie Université (NU)-École Nationale Supérieure d'Ingénieurs de Caen (ENSICAEN), Normandie Université (NU)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire SUBATECH Nantes (SUBATECH), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Nantes (UN)-Mines Nantes (Mines Nantes), CSNSM AS, Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Physique théorique (THEORIE), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Normandie Université (NU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Mines Nantes (Mines Nantes)-Université de Nantes (UN)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, Excitation function, Elastic scattering, Nuclear and High Energy Physics, Proton, 010308 nuclear & particles physics, Scattering, Nuclear Theory, FOS: Physical sciences, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], Isotopes of sodium, 01 natural sciences, 23.50.+z, 24.30.-v, 25.60.Bx, 21.10.Tg, 0103 physical sciences, Nuclear Experiment (nucl-ex), Atomic physics, 010306 general physics, Spectroscopy, Nucleon, Nuclear Experiment, Isotopes of magnesium
Abstract

Expérience GANIL E521aS/SPIRAL; International audience; The unbound nucleus $^{18}$Na, the intermediate nucleus in the two-proton radioactivity of $^{19}$Mg, was studied by the measurement of the resonant elastic scattering reaction $^{17}$Ne(p,$^{17}$Ne)p performed at 4 A.MeV. Spectroscopic properties of the low-lying states were obtained in a R-matrix analysis of the excitation function. Using these new results, we show that the lifetime of the $^{19}$Mg radioactivity can be understood assuming a sequential emission of two protons via low energy tails of $^{18}$Na resonances.

Published
2012
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19. Astrophysical($\alpha$, $\gamma$) reaction in inverse kinematics; Electron screening effect in the beta-decay

Author

Vincent Tatischeff, O. Sorlin, Paraskevi Demetriou, A. Buta, M. A. Amthor, T. J. Mertzimekis, C. Borcea, R. Borcea, Alain Pautrat, O. Kamalou, L. Caceres, A. Lefebvre-Schuhl, Predrag Ujić, I. Deloncle, B. Bastin, Sotirios Harissopulos, C. Stodel, Eric Clément, A. Coc, M. G. Saint-Laurent, L. Achouri, M. Lewitowicz, F. de Oliveira, A. Spyrou, S. Grévy, L Perot, M. Assié, V. Méot, L. Gaudefroy, A. Lagoyannis, Jürgen Kiener, M. Stanoiu, A. Lepailleur, Grand Accélérateur National d'Ions Lourds (GANIL), Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), CSNSM AN, Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)-Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut de Physique Nucléaire d'Orsay (IPNO), Laboratoire de physique corpusculaire de Caen (LPCC), Université de Caen Normandie (UNICAEN), Normandie Université (NU)-Normandie Université (NU)-École Nationale Supérieure d'Ingénieurs de Caen (ENSICAEN), Normandie Université (NU)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire de cristallographie et sciences des matériaux (CRISMAT), École Nationale Supérieure d'Ingénieurs de Caen (ENSICAEN), Normandie Université (NU)-Normandie Université (NU)-Centre National de la Recherche Scientifique (CNRS)-Université de Caen Normandie (UNICAEN), Normandie Université (NU)-Institut de Chimie du CNRS (INC), CSNSM SNO, Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)-Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Vinča Institute of Nuclear Sciences, University of Belgrade [Belgrade], National Center for Scientific Research 'Demokritos' (NCSR), National Superconducting Cyclotron Laboratory (NSCL), Michigan State University [East Lansing], Michigan State University System-Michigan State University System, Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Normandie Université (NU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), IFIN-HH, Normandie Université (NU)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche sur les Matériaux Avancés (IRMA), Normandie Université (NU)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université de Rouen Normandie (UNIROUEN), Normandie Université (NU)-Institut national des sciences appliquées Rouen Normandie (INSA Rouen Normandie), Institut National des Sciences Appliquées (INSA)-Normandie Université (NU)-Institut National des Sciences Appliquées (INSA)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université de Rouen Normandie (UNIROUEN), Institut National des Sciences Appliquées (INSA)-Normandie Université (NU)-Institut National des Sciences Appliquées (INSA)-Centre National de la Recherche Scientifique (CNRS), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), and Direction des Applications Militaires (DAM)

Subjects
History, Particle physics and field theory, Nuclear physics, Electron, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], 7. Clean energy, 01 natural sciences, Education, Ion, symbols.namesake, Astrophysics and astroparticles, 0103 physical sciences, Coulomb, Nuclear fusion, 010306 general physics, Debye, Superconductivity, Physics, 010308 nuclear & particles physics, Screening effect, Computer Science Applications, 13. Climate action, symbols, 23.40.-s, 25.75.-q, 21.60.Gx, 27.10.+h, 24.10.Ht, 95.30.Cq, Atomic physics, Beam (structure)
Abstract

International audience; The abundance calculations of the p-nuclei produced in explosive stellar sites rely on the Hauser-Feshbach (HF) theory with the alpha-article optical model potential (α-OMP) one of its major ingredients. To date, most of the (α, γ) cross sections measured show that HF calculations can be wrong by a factor of ten or more especially when phenomenological α-OMP are employed. To investigate the relevant uncertainties entering the HF calculations and furthermore develop global microscopic α-OMPs, systematic (α, γ) cross-section measurements are necessary. This led us to perform a feasibility study of (α, γ) measurements in inverse kinematics that will allow us to employ also radioactive beams in the future. Hence, the 4He(78Kr,γ)82Sr reaction was studied using the LISE3 spectrometer to separate the 82Sr recoils from the primary 78Kr beam. Although an excellent rejection factor > 1010 was achieved, the position of the ions of interest was unexpectedly masked by a secondary beam of high intensity. Given these, new setup improvements are proposed to remove the pollutant ions. Recently, many experiments were conducted in order to study the influence of the environment (especially in a metallic material) on the decay probability of radioactive nuclei. Additionally, hydrogen-like fusion reactions were performed indicating a change in the cross-section due to the influence of the Coulomb field screening induced by quasi-free electrons in metals. This was explained by the Debye screening model which treats metallic electrons within Maxwell-Boltzmann statistics. We measured the decay rate of 19O in metallic, insulating and superconducting environments whereas the electrons in the superconductors should obey the Bose-Einstein statistics. The decay rate measurement was supported by a branching ratios measurement. We found that the effect on the decay rate, if any, is less than the 0.1%, far below the theoretical predictions.

Published
2011
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20. Measurements of nuclearγ-ray line emission in interactions of protons andαparticles with N, O, Ne, and Si

Author

J.-P. Thibaud, J. C. Dalouzy, N. de Séréville, Vincent Tatischeff, S. Ouichaoui, H. Benhabiles-Mezhoud, Jürgen Kiener, A. Coc, F. Dayras, I. Deloncle, F. de Grancey, Livio Lamia, M. G. Pellegriti, J. Duprat, A. Lefebvre-Schuhl, C. Hamadache, and F. de Oliveira

Subjects
Nuclear reaction, Physics, Nuclear and High Energy Physics, Proton, 010308 nuclear & particles physics, Alpha particle, Coupling (probability), 01 natural sciences, 7. Clean energy, Nuclear physics, 0103 physical sciences, Production (computer science), Isotopes of silicon, Atomic physics, Nuclear Experiment, 010303 astronomy & astrophysics, Energy (signal processing), Oxygen-16
Abstract

$\ensuremath{\gamma}$-ray production cross sections have been measured in proton irradiations of N, Ne, and Si and $\ensuremath{\alpha}$-particle irradiations of N and Ne. In the same experiment we extracted also line shapes for strong $\ensuremath{\gamma}$-ray lines of $^{16}\mathrm{O}$ produced in proton and $\ensuremath{\alpha}$-particle irradiations of O. For the measurements gas targets were used for N, O, and Ne and a thick foil for Si. All targets were of natural isotopic composition. Beams in the energy range up to 26 MeV for protons and 39 MeV for $\ensuremath{\alpha}$ particles were delivered by the Institut de Physique Nucl\'eaire--Orsay tandem accelerator. The $\ensuremath{\gamma}$ rays were detected with four high-purity Ge detectors in the angular range ${30}^{\ifmmode^\circ\else\textdegree\fi{}}$ to ${135}^{\ifmmode^\circ\else\textdegree\fi{}}$. We extracted 36 cross-section excitation functions for proton reactions and 14 for $\ensuremath{\alpha}$-particle reactions. For the majority of the excitation functions no other data exist to our knowledge. Where comparison with existing data was possible, usually a very good agreement was found. It is shown that these data are very interesting for constraining nuclear reaction models. In particular, the agreement of cross section calculations in the nuclear reaction code talys with the measured data could be improved by adjusting the coupling schemes of collective levels in the target nuclei $^{14}\mathrm{N}$, $^{20,22}\mathrm{Ne}$, and $^{28}\mathrm{Si}$. The importance of these results for the modeling of nuclear $\ensuremath{\gamma}$-ray line emission in astrophysical sites is discussed.

Published
2011
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21. Half-life measurements of 137,139Cs excited nuclear states

Author

P. Petkov, Ts. Venkova, María Angélica Cardona, Daniel Hojman, Jürgen Kiener, D. Tonev, I. Deloncle, B. Roussière, Institut de Physique Nucléaire d'Orsay (IPNO), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), CSNSM SNO, Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), and CSNSM AN

Subjects
Physics, Nuclear and High Energy Physics, 010308 nuclear & particles physics, Hadron, Photofission, Half-life, State (functional analysis), [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], 21.10.Tg − 25.85.Jg − 27.60.+j 90, 01 natural sciences, Measure (mathematics), Excited state, 0103 physical sciences, Nuclear fusion, Atomic physics, 010306 general physics, Spin (physics)
Abstract

A fast-timing setup has been developed to measure the nuclear-state half-lives of neutron-rich nuclei. The first on-line measurements were performed on 137, 139Cs obtained from the β decay of 137, 139Xe. These neutron-rich Xe nuclei were produced by the 238U photofission induced by the 50MeV electron beam delivered by the ALTO facility. The half-lives of the first excited state in 137Cs and of six excited states in 139Cs were measured for the first time. Taking into account new information given by the deduced transition probabilities, we discuss the structure of the first excited states in 137, 139Cs : it is shown that, in both nuclei, the first excited $$\tfrac{5} {2}^ +$$ level corresponds mainly to the one-proton state issued from the π2d 5/2 orbital and that the most probable spin values for the states located at 289.8, 393.5, and 393.8keV in 139Cs are $$\tfrac{5} {2}^ +$$ , $$\tfrac{3} {2}^ +$$ , and $$\tfrac{1} {2}^ +$$ , respectively.

Published
2011
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22. Direct measurement of the $^{18}$F$(p,\alpha)^{15}$O reaction for application to nova gamma-ray emission

Author

L. Achouri, Paul Mumby-Croft, I. Stefan, P. Leleux, Kelly Vaughan, Douglas Robertson, Nicolas de Séréville, Jürgen Kiener, Pierre Descouvemont, E. Casarejos, N. A. Orr, A. Coc, F. Hammache, Vincent Tatischeff, T. Davinson, A. Lefebvre-Schuhl, Alison Laird, S. P. Fox, Pierpaolo Figuera, C. Angulo, Université Catholique de Louvain = Catholic University of Louvain (UCL), Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut de Physique Nucléaire d'Orsay (IPNO), Laboratoire de physique corpusculaire de Caen (LPCC), Université de Caen Normandie (UNICAEN), Normandie Université (NU)-Normandie Université (NU)-École Nationale Supérieure d'Ingénieurs de Caen (ENSICAEN), Normandie Université (NU)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Grand Accélérateur National d'Ions Lourds (GANIL), Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Normandie Université (NU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and Guesnon, Sandrine

Subjects
Physics, Astrophysics and Astronomy, [PHYS.NEXP] Physics [physics]/Nuclear Experiment [nucl-ex], 010308 nuclear & particles physics, Radiochemistry, Gamma ray, Alpha (ethology), Nova (laser), [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], 7. Clean energy, 01 natural sciences, 13. Climate action, 0103 physical sciences, 010303 astronomy & astrophysics
Abstract

International audience; The 18F nucleus is one of the radioactive isotopes produced during nova explosions. It is of particular interest since it is mainly responsible for the 511 keV gamma-ray emission of novae that could be detected with the INTEGRAL satellite or future gamma-ray telescopes. The amount of 18F synthesised still suffers from large uncertainties coming from missing nuclear information concerning the 18F destruction reaction 18F(p,a)15O. In particular, the interference sign between three 3/2+ resonances in 19Ne, situated slightly above the proton threshold (8 keV and/or 38 keV) and at higher energy (665 keV), is unknown. The maximum effect of these interferences is lying in the energy range corresponding to the Gamow peak region and has a strong impact on the 18F(p,a)15O reaction rate. We report here on the direct measurement at low energy (down to 400 keV in the center-of-mass) of the 18F(p,a)15O total cross section that we performed at the Louvain-la-Neuve CRC-RIB facility with the high-intensity and -purity 18F radioactive beam (T1/2 = 110 min). The total cross section for the different incident energies will be presented and compared to previous experimental data.

Published
2010
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23. Fast timing: Lifetime measurements with LaBr3 scintillators

Author

P. Petkov, María Angélica Cardona, B. Roussière, Jürgen Kiener, Daniel Hojman, I. Deloncle, Dimitar Tonev, Ts. Venkova, Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and Institut de Physique Nucléaire d'Orsay (IPNO)

Subjects
History, Ciencias Físicas, Física Nuclear, Measure (physics), Scintillator, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], 01 natural sciences, 7. Clean energy, Education, Nuclear physics, Optics, PHOTOMULTIPLIER, 0103 physical sciences, DETECTORS, 010306 general physics, BETA DECAY, PHOTOFISSION, Line (formation), Physics, FAST TIMING TECHNIQUE, 010308 nuclear & particles physics, business.industry, Photofission, Time resolution, Computer Science Applications, NEUTRON RICH NUCLEI, RESOLUTION, Cathode ray, business, Intensity (heat transfer), CIENCIAS NATURALES Y EXACTAS
Abstract

In order to perform half-life measurements at Alto, we developed a fast-timing setup using fast scintillators : LaBr3. The main components of our setup and their characteristics (timing properties) are presented. The resulting time resolution, obtained after optimization, and measured off-line with radioactive sources is discussed. This set-up was tested on-line by measuring using the slope method half-lives of 137-139Cs levels fed by the β- decay of 137-139Xe. The neutron-rich Xe nuclei were produced by 238U photofission using, at low intensity, the electron beam and the line of the future facility ALTO. Our results show the ability of such a fast-timing system to measure half-lives lower than the total time resolution. Off-line and on-line results are discussed. Fil: Deloncle, I.. Université Paris Sud; Francia. Centre National de la Recherche Scientifique; Francia Fil: Roussière, B.. Centre National de la Recherche Scientifique; Francia. Université Paris Sud; Francia Fil: Cardona, Maria Angelica. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Comision Nacional de Energia Atomica. Gerencia D/area Invest y Aplicaciones No Nucleares. Gerencia Fisica (cac). Departamento de Física de la Materia Condensada.; Argentina Fil: Hojman, Daniel Leonardo. Comision Nacional de Energia Atomica. Gerencia D/area Invest y Aplicaciones No Nucleares. Gerencia Fisica (cac). Departamento de Física de la Materia Condensada.; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina Fil: Kiener, J.. Université Paris Sud; Francia. Centre National de la Recherche Scientifique; Francia Fil: Petkov, P.. Institue of Nuclear Research and Nuclear Energy; Bulgaria Fil: Tonev, D.. Institue of Nuclear Research and Nuclear Energy; Bulgaria Fil: Venkova, Ts.. Institue of Nuclear Research and Nuclear Energy; Bulgaria

Published
2010
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24. Discovery of a New Broad Resonance inNe19: Implications for the Destruction of the Cosmicγ-Ray EmitterF18

Author

A. Coc, M. Stanoiu, I. Stefan, F. Negoita, R. Borcea, Jürgen Kiener, J. C. Dalouzy, F. de Oliveira Santos, A. M. Sánchez-Benítez, P. J. Woods, N. de Séréville, C. Borcea, H. Benhabiles, P. Bourgault, A. Damman, A. Buta, Marialuisa Aliotta, O. Sorlin, L. Achouri, M. G. Pellegriti, Carmen Angulo, F. de Grancey, and Thomas Davinson

Subjects
Physics, Degree (graph theory), 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Zero (complex analysis), General Physics and Astronomy, Resonance, Inelastic scattering, 01 natural sciences, Angular correlation, 0103 physical sciences, Atomic physics, Proton emission, Nuclear Experiment, 010306 general physics, Spin-½
Abstract

Six proton-emitting states in $^{19}\mathrm{Ne}$ were studied through the inelastic scattering reaction $\mathrm{H}(^{19}\mathrm{Ne},p)^{19}\mathrm{Ne}^{*}(p)^{18}\mathrm{F}$. Their energies and widths were derived from the protons detected at zero degree, while proton-proton angular correlations between the detector at zero degree and a segmented annular detector were used to determine their spin value. In addition to the known states, a new broad $J=\frac{1}{2}$ resonance has been evidenced at ${E}_{x}\ensuremath{\approx}7.9\text{ }\text{ }\mathrm{MeV}$, $\ensuremath{\approx}1.45\text{ }\text{ }\mathrm{MeV}$ above the proton emission threshold. By introducing this resonance, the $^{18}\mathrm{F}(p,\ensuremath{\alpha})^{15}\mathrm{O}$ destruction rate in novae is significantly enhanced. This reduces the chance to observe the cosmic $\ensuremath{\gamma}$-ray emission of $^{18}\mathrm{F}$ from novae in space telescopes.

Published
2009
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25. Indirect study of12C(α,γ)16O reaction

Author

Pierre Descouvemont, D. Beaumel, P. Roussel, A. Bouda, S. Fortier, L. Audouin, A. Lefebvre-Schuhl, N. Oulebsir, L. Gaudefroy, M. G. Pellegriti, F. Hammache, V. Tatischeff, and Jürgen Kiener

Subjects
History, 010308 nuclear & particles physics, Radiative capture, Extrapolation, chemistry.chemical_element, 01 natural sciences, Physique atomique et nucléaire, Computer Science Applications, Education, Stars, Cross section (physics), chemistry, 0103 physical sciences, Atomic physics, 010306 general physics, Helium
Abstract

The radiative capture reaction 12C(α,γ)16O plays an important role in helium burning in massive stars and their subsequent evolution [1]. However, despite various experimental studies, the cross section of this reaction at stellar energies remains highly uncertain. The extrapolation down to stellar energy (Ecm∼300 keV) of the measured cross sections at higher energies is made difficult by the overlap of various contributions of which some are badly known such as that of the 2+ (Ex=6.92 MeV) and 1- (Ex=7.12 MeV) sub-threshold states of 16O. Hence, to further investigate the contribution of these two-subthreshold resonances to the 12C(α,γ)16O cross section, a new determination of their a-reduced widths and so their a- spectroscopic-factors was performed using 12C(7Li,t)16O transfer reaction measurements at two incident energies and a detailed DWBA analysis of the data [2]. The measured and calculated differential cross sections are presented as well as the obtained spectroscopic factors and the a- reduced widths as well as the assymptotic normalization constants (ANC) for the 2+ and 1- subthreshold states. Finally, the results obtained from the R-matrix calculations of the 12C(α,γ)16O cross section using our obtained a-reduced widths for the two sub-threshold resonances are presented and discussed., SCOPUS: cp.j, info:eu-repo/semantics/published

Published
2016
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26. New determinations of gamma-ray line intensities of the Ep = 550 keV and Ep = 1747 keV resonances of the 13-C(p,gamma)14-N reaction

Author

Vincent Tatischeff, I Bailly, A. Bauchet, C. Chapuis, G. Tauzin, I. Deloncle, Jürgen Kiener, M. Gros, Stéphane Schanne, N. de Séréville, Marie-Geneviève Porquet, Bertrand Cordier, and David Attié

Subjects
Nuclear reaction, Physics, Nuclear and High Energy Physics, Branching fraction, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, FOS: Physical sciences, Electromagnetic radiation, Spectral line, Particle detector, Semiconductor detector, Atomic physics, Nuclear Experiment (nucl-ex), Nuclear Experiment, Instrumentation, Beam (structure)
Abstract

Gamma-ray angular distributions for the resonances at Ep = 550 keV and 1747 keV of the radiative capture reaction 13-C(p,g)14-N have been measured, using intense proton beams on isotopically pure 13-C targets. Relative intensities for the strongest transitions were extracted with an accuracy of typically five per cent, making these resonances new useful gamma-ray standards for efficiency calibration in the energy range Egamma = 1.6 to 9 MeV., Comment: 17 pages, 6 figures, Nuclear Instruments and Methods, Sec. A, accepted

Published
2003
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27. First identification and modelling of SPI background lines

Author

David Attié, V. Lonjou, R. C. Reedy, J. P. Roques, M. Gros, M. J. Harris, Jürgen Knödlseder, Chris Shrader, Cornelia B. Wunderer, Steven J. Sturner, Vincent Tatischeff, Bonnard J. Teegarden, Pierre Leleux, C. Ferguson, V. Schönfelder, Jürgen Kiener, Roland Diehl, G. Vedrenne, Pierre Jean, G. Weidenspointner, Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), and Université Fédérale Toulouse Midi-Pyrénées

Subjects
Physics, Spacecraft, Spectrometer, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, business.industry, Astrophysics::High Energy Astrophysical Phenomena, Monte Carlo method, Highly elliptical orbit, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, methods: data analysis, methods: numerical, instrumentation: miscellaneous, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Identification (information), Space and Planetary Science, Observatory, 0103 physical sciences, business, 010303 astronomy & astrophysics, line: identification, Remote sensing
Abstract

On Oct. 17, 2002, the ESA INTEGRAL observatory was launched into a highly elliptical orbit. SPI, a high resolution Ge spectrometer covering an energy range of 20-8000 keV, is one of its two main instruments. We use data recorded early in the mission (i.e. in March 2003) to characterize the instrumental background, in particular the many gamma-ray lines produced by cosmic-ray interactions in the instrument and spacecraft materials. More than 300 lines and spectral features are observed, for about 220 of which we provide identifications. An electronic version of this list, which will be updated continuously, is available for download at CESR. We also report first results from our efforts to model these lines by ab initio Monte Carlo simulation.

Published
2003
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29. DE-EXCITATION NUCLEAR GAMMA-RAY LINE EMISSION FROM LOW-ENERGY COSMIC RAYS IN THE INNER GALAXY

Author

Jürgen Kiener, Andrew W. Strong, Vincent Tatischeff, and H. Benhabiles-Mezhoud

Subjects
Physics, Astrophysics::High Energy Astrophysical Phenomena, Interstellar cloud, Gamma ray, Astronomy and Astrophysics, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Spectral line, Interstellar medium, Space and Planetary Science, Emission spectrum, Nuclear Experiment, Nucleon, Astrophysics::Galaxy Astrophysics
Abstract

Recent observations of high ionization rates of molecular hydrogen in diffuse interstellar clouds point to a distinct low-energy cosmic-ray component. Supposing that this component is made of nuclei, two models for the origin of such particles are explored and low-energy cosmic-ray spectra are calculated, which, added to the standard cosmic-ray spectra, produce the observed ionization rates. The clearest evidence of the presence of such low-energy nuclei between a few MeV nucleon{sup -1} and several hundred MeV nucleon{sup -1} in the interstellar medium would be a detection of nuclear {gamma}-ray line emission in the range E {sub {gamma}} {approx} 0.1-10 MeV, which is strongly produced in their collisions with the interstellar gas and dust. Using a recent {gamma}-ray cross section compilation for nuclear collisions, {gamma}-ray line emission spectra are calculated alongside the high-energy {gamma}-ray emission due to {pi}{sup 0} decay, the latter providing normalization of the absolute fluxes by comparison with Fermi-LAT observations of the diffuse emission above E {sub {gamma}} = 0.1 GeV. Our predicted fluxes of strong nuclear {gamma}-ray lines from the inner Galaxy are well below the detection sensitivities of the International Gamma-Ray Astrophysics Laboratory, but a detection, especially of the 4.4 MeV line, seems possible with new-generationmore » {gamma}-ray telescopes based on available technology. We also predict strong {gamma}-ray continuum emission in the 1-8 MeV range, which, in a large part of our model space for low-energy cosmic rays, considerably exceeds the estimated instrument sensitivities of future telescopes.« less

Published
2013
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30. Fast-timing measurements performed at ALTO on137,139Cs

Author

Jürgen Kiener, Daniel Hojman, María Angélica Cardona, P. Petkov, I. Deloncle, B. Roussière, Dimitar Tonev, and Ts. Venkova

Subjects
Physics, Nuclear physics, History, Excited state, Photofission, Cathode ray, Neutron, Atomic physics, Spin (physics), Open shell, Computer Science Applications, Education
Abstract

Fast-timing measurements were performed on 137,139Cs obtained from the ?? decay of 137'139Xe. The neutron-rich Xe nuclei were produced by the 238IJ photofission induced by the 50 MeV electron beam delivered by the ALTO facility. The half-lives of the first excited state in 137Cs and of six excited states in 139Cs were measured for the first time. These T1/2 results give new information on the structure of the 137,13955Cs82,84 nuclei located near the neutron closed shell N = 82. In particular, it is shown that, in both nuclei, the first excited 5/2+ level corresponds mainly to the one-proton state issued from the ?2d5/2 orbital. From the comparison with other N = 84 isotones, the most probable spin values for the states located at 289.8, 393.5, and 393.8 keV in 139Cs appear to be 5/2+, 3/2+, and 1/2+.

Published
2012
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31. GRIPS - Gamma-Ray Imaging, Polarimetry and Spectroscopy

Author

L. G. Balasz, Jürgen Kiener, Wlodek Klamra, Gennady S. Bisnovatij-Kogan, Asaf Pe'er, Friedrich-Karl Thielemann, Grzegorz Wrochna, Suzanne Foley, Wolfgang Rhode, G. DiCocco, Claes Fransson, Claudio Labanti, Andrzej A. Zdziarski, Georg G. Raffelt, Olaf Reimer, Wolfgang Hillebrandt, Attila Mészáros, Boris Shustov, Elena Pian, Omar Tibolla, Jochen Greiner, Stefan Larsson, Matthias Kadler, Joachim Trümper, Lorraine Hanlon, David Tierney, Jordi José, W. Hermsen, Lucien Kuiper, Radoslaw Marcinkowski, Neil Gehrels, Andrej Bykov, Shawn Bishop, Nikos Prantzos, Sheila McBreen, Roland Diehl, Steven E. Boggs, Felix Ryde, Mark Pearce, Keiichi Maeda, A. F. Iyudin, Martino Marisaldi, Jörn Wilms, Ingo Kreykenbohm, Felix Aharonian, Guido Barbiellini, Ronaldo Bellazzini, Uwe Laux, Nikolaos D. Kylafis, Nial R. Tanvir, G. Kanbach, Ken'ichi Nomoto, Norbert Langer, Christian Schmidt, Marco Ajello, Dominik Elsässer, K. Langanke, K. Mannheim, Andrew W. Strong, Bruno Leibundgut, Andreas Zoglauer, Sylvio Klose, D. A. Varshalovich, B. McBreen, René Hudec, Francesco Longo, Joseph Silk, Dieter H. Hartmann, Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Greiner, Jochen, Mannheim, Karl, Aharonian, Felix, Ajello, Marco, Balasz Lajos, G., Barbiellini, Guido, Bellazzini, Ronaldo, Bishop, Shawn, Bisnovatij Kogan Gennady, S., Boggs, Steven, Bykov, Andrej, Dicocco, Guido, Diehl, Roland, Elsässer, Dominik, Foley, Suzanne, Fransson, Clae, Gehrels, Neil, Hanlon, Lorraine, Hartmann, Dieter, Hermsen, Wim, Hillebrandt, Wolfgang, Hudec, Rene, Iyudin, Anatoli, Jose, Jordi, Kadler, Matthia, Kanbach, Gottfried, Klamra, Wlodek, Kiener, Jürgen, Klose, Sylvio, Kreykenbohm, Ingo, Kuiper Lucien, M., Kylafis, Niko, Labanti, Claudio, Langanke, Karlheinz, Langer, Norbert, Larsson, Stefan, Leibundgut, Bruno, Laux, Uwe, Longo, Francesco, Maeda, Kei'Ichi, Marcinkowski, Radoslaw, Marisaldi, Martino, Mcbreen, Brian, Mcbreen, Sheila, Meszaros, Attila, Nomoto, Ken'Ichi, Pearce, Mark, Peer, Asaf, Pian, Elena, Prantzos, Nikola, Raffelt, Georg, Reimer, Olaf, Rhode, Wolfgang, Ryde, Felix, Schmidt, Christian, Silk, Joe, Shustov Boris, M., Strong, Andrew, Tanvir, Nial, Thielemann Friedrich, Karl, Tibolla, Omar, Tierney, David, Trümper, Joachim, Varshalovich Dmitry, A., Wilms, Jörn, Wrochna, Grzegorz, Zdziarski, Andrzej, Zoglauer, Andreas, and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Cosmic Vision, gamma-ray satellites, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Magnetar, 7. Clean energy, 01 natural sciences, Early Universe, Polarization, 0103 physical sciences, Nuclear astrophysics, Blazar, 010303 astronomy & astrophysics, media_common, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, gamma-ray satellite, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Gamma-ray Bursts, Galaxy, Universe, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Supernova, 13. Climate action, Space and Planetary Science, Compton and Pair creation telescope, Gamma-ray bursts, Neutrino, Astrophysics - High Energy Astrophysical Phenomena, Nucleosynthesis
Abstract

We propose to perform a continuously scanning all-sky survey from 200 keV to 80 MeV achieving a sensitivity which is better by a factor of 40 or more compared to the previous missions in this energy range. The Gamma-Ray Imaging, Polarimetry and Spectroscopy (GRIPS) mission addresses fundamental questions in ESA's Cosmic Vision plan. Among the major themes of the strategic plan, GRIPS has its focus on the evolving, violent Universe, exploring a unique energy window. We propose to investigate $\gamma$-ray bursts and blazars, the mechanisms behind supernova explosions, nucleosynthesis and spallation, the enigmatic origin of positrons in our Galaxy, and the nature of radiation processes and particle acceleration in extreme cosmic sources including pulsars and magnetars. The natural energy scale for these non-thermal processes is of the order of MeV. Although they can be partially and indirectly studied using other methods, only the proposed GRIPS measurements will provide direct access to their primary photons. GRIPS will be a driver for the study of transient sources in the era of neutrino and gravitational wave observatories such as IceCUBE and LISA, establishing a new type of diagnostics in relativistic and nuclear astrophysics. This will support extrapolations to investigate star formation, galaxy evolution, and black hole formation at high redshifts., Comment: to appear in Exp. Astron., special vol. on M3-Call of ESA's Cosmic Vision 2010; 25 p., 25 figs; see also www.grips-mission.eu

Published
2011
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