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4 results on '"K. E. Rehm"'

1. Reaction rate for carbon burning in massive stars

Author

Xiao Fang, Rashi Talwar, John P. Greene, Martín Alcorta, Claudio Ugalde, T. Lauritsen, Brian Bucher, Kalle Auranen, A. D. Ayangeakaa, S. Zhu, B. P. Kay, D. Seweryniak, S. T. Marley, B. B. Back, M. Heine, C. L. Jiang, J. Sethi, L. Morris, D. Bourgin, D. Montanari, A. Lefebvre-Schuhl, S. Bottoni, F. Haas, Clayton Dickerson, Sergio Almaraz-Calderon, K. E. Rehm, D. G. Jenkins, G. Fruet, S. A. Kuvin, B. DiGiovine, C. M. Deibel, C. R. Hoffman, Daniel Santiago-Gonzalez, S. Courtin, R. C. Pardo, X. Tang, M. P. Carpenter, R. V. F. Janssens, Melina Avila, Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-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), Université de Strasbourg (UNISTRA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), 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, Fusion, Isotope, 010308 nuclear & particles physics, S-factor, chemistry.chemical_element, 7. Clean energy, 01 natural sciences, Reaction rate, Nuclear physics, Critical phase, Stars, Physique [physics]/Astrophysique [astro-ph], chemistry, 13. Climate action, Nucleosynthesis, 0103 physical sciences, lipids (amino acids, peptides, and proteins), 010306 general physics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Carbon
Abstract

International audience; Carbon burning is a critical phase for nucleosynthesis in massive stars. The conditions for igniting this burning stage, and the subsequent isotope composition of the resulting ashes, depend strongly on the reaction rate for C12+C12 fusion at very low energies. Results for the cross sections for this reaction are influenced by various backgrounds encountered in measurements at such energies. In this paper, we report on a new measurement of C12+C12 fusion cross sections where these backgrounds have been minimized. It is found that the astrophysical S factor exhibits a maximum around Ecm=3.5–4.0 MeV, which leads to a reduction of the previously predicted astrophysical reaction rate.

Published
2018

2. Cross section measurements in the $^{12}$C+$^{12}$C system

Author

S. Della Negra, Sergio Almaraz-Calderon, Oliver S. Kirsebom, B. Bucher, C. L. Jiang, R. V. F. Janssens, Anne Meyer, Rashi Talwar, X.D. Tang, John P. Greene, B. B. Back, M. Heine, G. Fruet, X. Fang, Fairouz Hammache, D. J. Henderson, S. A. Kuvin, P. Adsley, Catherine Deibel, M. Rudigier, Kalle Auranen, S. Zhu, S. Courtin, M. Albers, D. Bourgin, M. P. Carpenter, Martín Alcorta, D. Seweryniak, Daniel Santiago-Gonzalez, D. Montanari, F. Haas, B. P. Kay, Calem Hoffman, P. H. Regan, D. G. Jenkins, P. F. Bertone, J. Sethi, C. Stodel, Claudio Ugalde, A. Lefebvre-Schuhl, J. Lesrel, A. D. Ayangeakaa, Clayton Dickerson, K. E. Rehm, B. DiGiovine, L. Morris, N. de Séréville, R. C. Pardo, Melina Avila, T. Lauritsen, S. Bottoni, S. T. Marley, Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-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), 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), 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), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-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 Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, 010308 nuclear & particles physics, QC1-999, Measure (physics), Aucun, chemistry.chemical_element, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], 01 natural sciences, Coincidence, law.invention, Nuclear physics, Ignition system, Cross section (physics), chemistry, 13. Climate action, law, 0103 physical sciences, Nuclear astrophysics, Nuclear fusion, 010306 general physics, Carbon
Abstract

International audience; The 12C+12C fusion reaction is one of the most important for nuclear astrophysics since it determines the carbon ignition in stellar environments. Two experiments which make use of the gamma-particle coincidence technique to measure the 12C+12C S-factors at deep sub barrier energies are discussed. Results are presented showing a decrease of the S-factor below Ec.m. = 3 MeV.

Published
2017

3. Fusion measurements of $^{12}$C+$^{12}$C at energies of astrophysical interest

Author

T. Lauritsen, R. V. F. Janssens, D. J. Henderson, B. B. Back, Martín Alcorta, K. E. Rehm, C. L. Jiang, Sergio Almaraz-Calderon, Xiao Fang, R. C. Pardo, B. DiGiovine, John P. Greene, Brian Bucher, J. Lai, D. Seweryniak, D. Montanari, X. D. Tang, A. Lefebvre-Schuhl, M. Paul, Clayton Dickerson, Daniel Santiago-Gonzalez, Melina Avila, Claudio Ugalde, A. D. Ayangeakaa, H. M. David, S. Zhu, S. Courtin, F. Haas, D. G. Jenkins, Catherine Deibel, M. P. Carpenter, D. Bourgin, Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-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), Université de Strasbourg (UNISTRA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), 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, Fusion, Range (particle radiation), 010308 nuclear & particles physics, QC1-999, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], 01 natural sciences, 7. Clean energy, Coincidence, Nuclear physics, Supernova, Cross section (physics), Stellar nucleosynthesis, 0103 physical sciences, Nuclear fusion, Gammasphere, 010306 general physics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; The cross section of the ^12C+^12C fusion reaction at low energies is of paramount importance for models of stellar nucleosynthesis in different astrophysical scenarios, such as Type Ia supernovae and Xray superbursts, where this reaction is a primary route for the production of heavier elements. In a series of experiments performed at Argonne National Laboratory, using Gammasphere and an array of Silicon detectors, measurements of the fusion cross section of ^12C+^12C were successfully carried out with the gamma and charged-particle coincidence technique in the center-of-mass energy range of 3-5 MeV. These were the first background-free fusion cross section measurements for ^12C+^12C at energies of astrophysical interest. Our results are consistent with previous measurements in the high-energy region; however, our lowest energy measurement indicates a fusion cross section slightly lower than those obtained with other techniques.

Published
2015

4. Fusion reactions of $^{58,64}Ni$+$^{124}Sn$

Author

F. Galtarossa, F. Haas, Suzana Szilner, T. Mijiatovic, E. Fioretto, Alain Goasduff, M. Mazzocco, R. N. Sagaidak, Henning Esbensen, Fernando Scarlassara, D. Montanari, C. L. Jiang, E. Strano, L. Corradi, Melina Avila, A. M. Stefanini, D. Bourgin, B. B. Back, S. Courtin, Daniel Santiago-Gonzalez, G. Montagnoli, S. Almaraz Calderon, K. E. Rehm, Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-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), and Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, Nuclear reaction, Coupling, Fusion, 010308 nuclear & particles physics, QC1-999, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], 01 natural sciences, Molecular physics, Nuclear physics, transfer reactions, spectrometers, Physics and Astronomy (all), nuclear reactions, fusion, 0103 physical sciences, Nuclear fusion, 010306 general physics
Abstract

Measurements of fusion excitation functions of Ni58+Sn124 and Ni64+Sn124 are extended towards lower energy to cross sections of 1 μb and are compared to detailed coupled-channels calculations. The calculations clearly show the importance of including transfer reactions in a coupled-channels treatment for such heavy systems. This result is different from the conclusion made in a previous article which claimed that the influence of transfer on fusion is not important for fusion reactions of Ni+Sn. In the energy region studied in this experiment no indication of fusion hindrance has been observed, which is consistent with a systematic study of this behavior.

Published
2015

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