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Journal articles on the topic 'Experimental nuclear astrophysic'

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Published: 9 March 2023

Last updated: 10 March 2023

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1

RAUSCHER, THOMAS. "THE PATH TO IMPROVED REACTION RATES FOR ASTROPHYSICS." International Journal of Modern Physics E 20, no. 05 (May 2011): 1071–169. http://dx.doi.org/10.1142/s021830131101840x.

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This review focuses on nuclear reactions in astrophysics and, more specifically, on reactions with light ions (nucleons and α particles) proceeding via the strong interaction. It is intended to present the basic definitions essential for studies in nuclear astrophysics, to point out the differences between nuclear reactions taking place in stars and in a terrestrial laboratory, and to illustrate some of the challenges to be faced in theoretical and experimental studies of those reactions. The discussion revolves around the relevant quantities for astrophysics, which are the astrophysical reaction rates. The sensitivity of the reaction rates to the uncertainties in the prediction of various nuclear properties is explored and some guidelines for experimentalists are also provided.

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2

CHAMPAGNE, A. E., and C. ILIADIS. "FIRST RESULTS FROM LENA." Modern Physics Letters A 22, no. 04 (February 10, 2007): 243–57. http://dx.doi.org/10.1142/s0217732307022724.

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We review the first results from the Laboratory for Experimental Nuclear Astrophysics (LENA), which is a dedicated accelerator facility for measuring reactions of astrophysical interest. We also briefly describe the facility itself and the detector system. The reactions that have been measured have relevance for both stellar evolution and for classical nova explosions.

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3

Shotter, A. C. "Experimental Nuclear Physics for Astrophysics." EAS Publications Series 11 (2004): 191–97. http://dx.doi.org/10.1051/eas:2004013.

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4

Wiescher, M. "Experimental Challenges in Nuclear Astrophysics." Nuclear Physics A 751 (April 2005): 285–300. http://dx.doi.org/10.1016/j.nuclphysa.2005.02.110.

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5

Prati, Paolo. "Underground Nuclear Astrophysics: pushing direct measurements toward the Gamow window." EPJ Web of Conferences 227 (2020): 01015. http://dx.doi.org/10.1051/epjconf/202022701015.

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The aim of experimental nuclear astrophysics is to provide information on the nuclear processes involved in astrophysical scenarios at the relevant energy range. However, the measurement of the cross section of nuclear reactions at low energies present formidable difficulties due to the very low reaction rates often overwhelmed by the background. Several approaches have been proposed and exploited to overcome such severe obstacles: in such frame, the idea to install a low energy - high intensity ion accelerator deep underground, to gain high luminosity while reducing the cosmic ray background, brought more than 25 years ago, to the pilot LUNA experiment. LUNA stands for Laboratory for Underground Nuclear Astrophysics: in the cave under the Gran Sasso mountain (in Italy) first a 50 kV and then a 400 kV single-ended accelerator for protons and alphas were deployed and produced plenty of data mainly on reactions of the H-burning phase in stars. Recently, similar facilities have been installed and/or proposed in other underground laboratories in US and China. LUNA as well is going to make a big step forward, with a new machine in the MV range which will be able to provide intense beams of protons, alphas and carbon ions. The rationale of underground nuclear astrophysics will be presented together with the last updates on the ongoing research programs.

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6

Rolfs, Claus. "Data needs in experimental nuclear astrophysics." Nuclear Physics News 4, no. 1 (January 1994): 17–20. http://dx.doi.org/10.1080/10506899408210217.

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7

Bardayan, D. W. "Recent Experimental Progress in Nuclear Astrophysics." Physics Procedia 66 (2015): 457–64. http://dx.doi.org/10.1016/j.phpro.2015.05.058.

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8

Aliotta, Marialuisa. "Experimental Nuclear Astrophysics in Underground Laboratories." Nuclear Physics News 22, no. 2 (May 31, 2012): 13–17. http://dx.doi.org/10.1080/10619127.2012.683715.

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Cavanna, Francesca, and Paolo Prati. "Direct measurement of nuclear cross-section of astrophysical interest: Results and perspectives." International Journal of Modern Physics A 33, no. 09 (March 30, 2018): 1843010. http://dx.doi.org/10.1142/s0217751x18430108.

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Stellar evolution and nucleosynthesis are interconnected by a wide network of nuclear reactions: the study of such connection is usually known as nuclear astrophysics. The main task of this discipline is the determination of nuclear cross-section and hence of the reaction rate in different scenarios, i.e. from the synthesis of a few very light isotopes just after the Big Bang to the heavy element production in the violent explosive end of massive stars. The experimental determination of reaction cross-section at the astrophysical relevant energies is extremely difficult, sometime impossible, due to the Coulomb repulsion between the interacting nuclei which turns out in cross-section values down to the fbar level. To overcome these obstacles, several experimental approaches have been developed and the adopted techniques can be roughly divided into two categories, i.e. direct and indirect methods. In this review paper, the general problem of nuclear astrophysics is introduced and discussed from the point of view of experimental approach. We focus on direct methods and in particular on the features of low-background experiments performed at underground laboratory facilities. The present knowledge of reactions involved in the Big Bang and stellar hydrogen-burning scenarios is discussed as well as the ongoing projects aiming to investigate mainly the helium- and carbon-burning phases. Worldwide, a new generation of experiment in the MeV range is in the design phase or at the very first steps and decisive progresses are expected to come in the next years.

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Frebel, Anna. "From Nuclei to the Cosmos: Tracing Heavy-Element Production with the Oldest Stars." Annual Review of Nuclear and Particle Science 68, no. 1 (October 19, 2018): 237–69. http://dx.doi.org/10.1146/annurev-nucl-101917-021141.

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Understanding the origin of the elements has been a decades-long pursuit, with many open questions remaining. Old stars found in the Milky Way and its dwarf satellite galaxies can provide answers because they preserve clean element abundance patterns of the nucleosynthesis processes that operated some 13 billion years ago, enabling reconstruction of the chemical evolution of the elements. This review focuses on the astrophysical signatures of heavy neutron-capture elements made in the s-, i-, and r-processes found in old stars. A highlight is the recently discovered r-process galaxy Reticulum II, which was enriched by a neutron star merger. These results show that old stars in dwarf galaxies provide a novel means to constrain the astrophysical site of the r-process, ushering in much-needed progress on this major outstanding question. This nuclear astrophysics research complements the many experimental and theoretical nuclear physics efforts into heavy-element formation, and also aligns with results on the gravitational-wave signature of neutron star mergers.

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11

Su, Jun, Zhihong Li, Hao Zhang, Yunju Li, Ertao Li, Chen Chen, Yangping Shen, et al. "Measurement of the low energy ²⁵Mg(p,γ)²⁶Al resonances." EPJ Web of Conferences 260 (2022): 08002. http://dx.doi.org/10.1051/epjconf/202226008002.

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The cosmic 1.809 MeV γ-ray emitted by the radioactive nucleus 26Al in the Galaxy is one of the key observation targets of the γ-ray astronomy. The 26Al is mainly produced by the 25Mg(p,γ)26Al reaction in the stellar Mg-Al reaction cycle. At the astrophysical relevant temperatures, the reaction rates of 25Mg(p,γ)26Al are dominated by several narrow resonances at low energy. This work reports a measurement of the low energy 25Mg(p,γ)26Al resonances at Jinping Underground Nuclear Astrophysics experimental facility (JUNA) in the China Jinping Underground Laboratory (CJPL).

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12

Axiotis, M., A. Lagoyannis, G. Provatas, V. Foteinou, A. Karydas, V. Kantarelou, D. Bazzacco, et al. "New Instruments for Nuclear Astrophysics." HNPS Proceedings 23 (March 8, 2019): 8. http://dx.doi.org/10.12681/hnps.1900.

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A major task in experimental nuclear astrophysics is the measurement of cross sections of capture reactions. In the last years, the astrophysics group of NCSR “Demokritos” developed and used a method for conducting this kind of research using a 4π NaI γ-detector. Of great importance in this method is the determination of the efficiency of the detector, which depends on the average multiplicity of the γ-cascade de-exciting the entry state of the produced nucleus. Two new experimental setups have been studied and are in course of installation at the Tandem Laboratory of the Institute of Nuclear and Particle Physics of NCSR “Demokritos”, that will provide the possibility for conducting this kind of experiments inhouse. The first one is a new 14x14 inches NaI detector and the second is the BGO Ball of the GASP setup. These detector setups as well as their potential experimental use will be described in detail.

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13

Wiescher, Michael. "Experimental Needs and Opportunities in Nuclear Astrophysics." Journal of Physics: Conference Series 420 (March 25, 2013): 012135. http://dx.doi.org/10.1088/1742-6596/420/1/012135.

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14

Wiescher, Michael. "Goals and challenges in experimental nuclear astrophysics." EPL (Europhysics Letters) 109, no. 6 (March 1, 2015): 62001. http://dx.doi.org/10.1209/0295-5075/109/62001.

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15

Aliotta, M. "Experimental nuclear astrophysics with radioactive ion beams." European Physical Journal Special Topics 150, no. 1 (November 2007): 201–6. http://dx.doi.org/10.1140/epjst/e2007-00304-7.

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16

Bochum, C. Rolfs, C. Spitaleri Catania, and F. Terrasi Naples. "European summer school on experimental nuclear astrophysics." Nuclear Physics News 12, no. 1 (January 2002): 13. http://dx.doi.org/10.1080/10506890208235631.

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17

Bruno, C. G. "Experimental challenges in low-energy nuclear astrophysics." Journal of Physics: Conference Series 1078 (August 2018): 012007. http://dx.doi.org/10.1088/1742-6596/1078/1/012007.

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18

Fynbo, H. O. U. "Few-Body Problems in Experimental Nuclear Astrophysics." Few-Body Systems 54, no. 7-10 (February 10, 2013): 843–48. http://dx.doi.org/10.1007/s00601-013-0646-9.

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19

Kubono, Shigeru. "Frontier in Experimental Nuclear Astrophysics in Japan." Journal of Nuclear Science and Technology 39, sup2 (August 2002): 524–29. http://dx.doi.org/10.1080/00223131.2002.10875155.

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20

Mascali, David, Domenico Santonocito, Simone Amaducci, Lucio Andò, Vincenzo Antonuccio, Sándor Biri, Alfio Bonanno, et al. "A Novel Approach to β-Decay: PANDORA, a New Experimental Setup for Future In-Plasma Measurements." Universe 8, no. 2 (January 27, 2022): 80. http://dx.doi.org/10.3390/universe8020080.

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Theoretical predictions as well as experiments performed at storage rings have shown that the lifetimes of β-radionuclides can change significantly as a function of the ionization state. In this paper we describe an innovative approach, based on the use of a compact plasma trap to emulate selected stellar-like conditions. It has been proposed within the PANDORA project (Plasmas for Astrophysics, Nuclear Decay Observation and Radiation for Archaeometry) with the aim to measure, for the first time in plasma, nuclear β-decay rates of radionuclides involved in nuclear-astrophysics processes. To achieve this task, a compact magnetic plasma trap has been designed to reach the needed plasma densities, temperatures, and charge-states distributions. A multi-diagnostic setup will monitor, on-line, the plasma parameters, which will be correlated with the decay rate of the radionuclides. The latter will be measured through the detection of the γ-rays emitted by the excited daughter nuclei following the β-decay. An array of 14 HPGe detectors placed around the trap will be used to detect the emitted γ-rays. For the first experimental campaign three isotopes, 176Lu, 134Cs, and 94Nb, were selected as possible physics cases. The newly designed plasma trap will also represent a tool of choice to measure the plasma opacities in a broad spectrum of plasma conditions, experimentally poorly known but that have a great impact on the energy transport and spectroscopic observations of many astrophysical objects. Status and perspectives of the project will be highlighted in the paper.

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21

Khaliel, A., T. J. Mertzimekis, A. Psaltis, I. Psyrra, A. Kanellakopoulos, V. Lagaki, V. Foteinou, M. Axiotis, and S. Harrisopulos. "Experimental Investigation of radiative proton-capture reactions relevant to Nucleosynthesis." HNPS Proceedings 24 (April 1, 2019): 168. http://dx.doi.org/10.12681/hnps.1861.

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One of the primary objectives of the field of Nuclear Astrophysics is the study of the elemental and isotopic abundances in our solar system. Although a lot of progress has been made regarding a large number of nuclides, there is still a number of neutron-deficient nuclei, ie the p nuclei, which cannot be created via the s and r processes. These processes are responsible for the production of the bulk of heavy nuclides. The pre-explosive or explosive phases of massive stars are considered potential loci for p nuclides production via various combinations of photodisintegrations and nucleon captures, along with β+ decays and electron captures. For the study of the vast network of nuclear reactions (over 20'000) that are responsible for observed isotopic abundances, the statistical model of Hauser-Feshbach is employed. The model requires the knowledge of nuclear reaction cross sections, quantities that can be measured in the laboratory. In this work, we report on recent experimental attempts to measure such cross sections in radiative proton-capture reactions involving 107,109Ag near the astrophysically relevant energy window. Measurements have been performed at the Tandem Accelerator Laboratory of the N.S.C.R. “Demokritos”. The results are compared to various theoretical models, using the TALYS and EMPIRE codes, in an attempt to provide experimental input to astrophysical models.

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22

Naselli, Eugenia, David Mascali, Claudia Caliri, Giuseppe Castro, Luigi Celona, Alessio Galatá, Santo Gammino, et al. "Nuclear β-decays in plasmas: how to correlate plasma density and temperature to the activity." EPJ Web of Conferences 227 (2020): 02006. http://dx.doi.org/10.1051/epjconf/202022702006.

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Magnetized plasmas in compact traps may become experimental en-vironments for the investigation of nuclear beta-decays of astrophysical inter-est. In the framework of the project PANDORA (Plasmas for Astrophysics, Nuclear Decays Observation and Radiation for Archaeometry) the research ac-tivities are devoted to demonstrate the feasibility of an experiment aiming atmeasuring lifetimes of radionuclides of astrophysical interest when changing the charge state distribution of the in-plasma ions and the other plasma param- eters such as density and temperature. This contribution describes the multidi-agnostics setup now available at INFN-LNS, which allows unprecedented in-vestigations of magnetoplasmas properties in terms of density, temperature and charge state distribution (CSD). The setup includes an interfero-polarimeter for total plasma density measurement, a multi-X-ray detectors system for X-ray spectroscopy (including time resolved spectroscopy), an X-ray pin-hole camera for high-resolution 2D space resolved spectroscopy, a two-pin plasma-chamber immersed antenna for the detection of plasma radio-self-emission, and differ- ent spectrometers for the plasma-emitted visible light characterization. The setup is also suitable for other studies of astrophysical interest, such as turbulent plasma regimes dominated by the so-called Cyclotron Maser Instability, which is a typical kinetic turbulence occurring in astrophysical objects like magnetized stars, brown dwarfs, etc. A description of recent results about plasma parame- ters characterization in quiescent and turbulent Electron Cyclotron Resonance-heated plasmas will be given.

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23

Käppeler, F., F. K. Thielemann, and M. Wiescher. "CURRENT QUESTS IN NUCLEAR ASTROPHYSICS AND EXPERIMENTAL APPROACHES." Annual Review of Nuclear and Particle Science 48, no. 1 (December 1998): 175–251. http://dx.doi.org/10.1146/annurev.nucl.48.1.175.

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24

Kubono, Shigeru. "Frontier in Experimental Nuclear Astrophysics with RI Beams." Progress of Theoretical Physics Supplement 146 (2002): 237–46. http://dx.doi.org/10.1143/ptps.146.237.

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25

Piatti, D. "The Study of the ⁶Li(p,γ)⁷Be Reaction at LUNA." Journal of Physics: Conference Series 1668, no. 1 (October 1, 2020): 012034. http://dx.doi.org/10.1088/1742-6596/1668/1/012034.

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Abstract The 6Li(p,γ)7Be reaction is mainly involved in two astrophysical scenarios: the primordial nucleosynthesis and 6Li consumption in pre-main and main sequence stars. A recent measurement of 6Li(p,γ)7Be reaction S-factor reported a resonance-like structure at Ecm = 195 keV, which has not been confirmed neither by other direct measurements nor by theoretical calculations. A new experiment was performed at the Laboratory for Underground Nuclear Astrophysics (LUNA). The extremely low background environment allowed to measure the 6Li(p,γ)7Be cross section down to low energies with unprecedented sensitivity leading to clarify the existence of the claimed resonance. Details on the experimental setup and the preliminary results of the ongoing analysis are reported in this work.

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26

THIELEMANN, F. K., D. MOCELJ, I. PANOV, E. KOLBE, T. RAUSCHER, K. L. KRATZ, K. FAROUQI, et al. "THE R-PROCESS: SUPERNOVAE AND OTHER SOURCES OF THE HEAVIEST ELEMENTS." International Journal of Modern Physics E 16, no. 04 (May 2007): 1149–63. http://dx.doi.org/10.1142/s0218301307006587.

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Rapid neutron capture in stellar explosions is responsible for the heaviest elements in nature, up to Th , U and beyond. This nucleosynthesis process, the r-process, is unique in the sense that a combination of nuclear physics far from stability (masses, half-lives, neutron-capture and photodisintegration, neutron-induced and beta-delayed fission and last but not least neutrino-nucleus interactions) is intimately linked to ejecta from astrophysical explosions (core collapse supernovae or other neutron star related events). The astrophysics and nuclear physics involved still harbor many uncertainties, either in the extrapolation of nuclear properties far beyond present experimental explorations or in the modeling of multidimensional, general relativistic (neutrino-radiation) hydrodynamics with rotation and possibly required magnetic fields. Observational clues about the working of the r-process are mostly obtained from solar abundances and from the abundance evolution of the heaviest elements as a function of galactic age, as witnessed in old extremely metal-poor stars. They contain information whether the r-process is identical for all stellar events, how abundance features develop with galactic time and whether the frequency of r-process events is comparable to that of average core collapse supernovae - producing oxygen through titanium, as well as iron-group nuclei. The theoretical modeling of the r-process has advanced from simple approaches, where the use of static neutron densities and temperatures can aid to test the influence of nuclear properties far from stability on abundance features, to more realistic expansions with a given entropy, global neutron/proton ratio and expansion timescales, as expected from explosive astrophysical events. The direct modeling in astrophysical events such as supernovae still faces the problem whether the required conditions can be met.

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27

Demetriou, P. "Global predictions for astrophysics applications." HNPS Proceedings 13 (February 20, 2020): 18. http://dx.doi.org/10.12681/hnps.2953.

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Nuclear reaction rates play a crucial role in nuclear astrophysics. In the last decades there has been an enormous effort to measure reaction cross sections and extensive experimental databases have been compiled as a result. In spite of these efforts, most nuclear reaction network calculations still have to rely on theoretical predic- tions of experimentally unknown rates. In particular, in astrophysics applications such as the s-, r- and p-process nucleosynthesis involving a large number of nuclei and nuclear reactions (thousands). Moreover, most of the ingredients of the cal- culations of reaction rates have to be extrapolated to energy and/or mass regions that cannot be explored experimentally. For this reason it is important to develop global microscopic or semi-microscopic models of nuclear properties that give an accurate description of existing data and are reliable for predictions far away from the stability line. The need for more microscopic input parameters has led to new devel- opments within the Hartree-Fock-Bogoliubov method, some of which are presented in this paper.

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28

Claudio, Spitaleri, Lamia Livio, and Pizzone Rosario Gianluca. "Preface: Eighth European Summer School on Experimental Nuclear Astrophysics." Journal of Physics: Conference Series 703 (April 2016): 011003. http://dx.doi.org/10.1088/1742-6596/703/1/011003.

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29

Wiescher, M. "Advances in experimental techniques and facilities for nuclear astrophysics." Nuclear Physics A 688, no. 1-2 (May 2001): 241–48. http://dx.doi.org/10.1016/s0375-9474(01)00707-2.

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30

Motobayashi, Tohru. "Experimental Studies of Nuclear Astrophysics with Fast RI beams." Journal of Nuclear Science and Technology 39, sup2 (August 2002): 558–61. http://dx.doi.org/10.1080/00223131.2002.10875162.

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31

Mrazek, J., V. Burjan, V. Kroha, A. M. Mukhamedzhanov, R. Tribble, C. Spitaleri, I. Siváček, et al. "ANC experiments for nuclear astrophysics in NPI CAS." EPJ Web of Conferences 184 (2018): 01014. http://dx.doi.org/10.1051/epjconf/201818401014.

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Asymptotic Normalization Coefficients method is one of the indirect methods used in nuclear astrophysics. The method allows to deduce a direct part of a radiative capture cross section from the measurement of a two body reaction under specific conditions. The experimental works started in collaboration of NPI CAS, TAMU and INFN LNS from 90-ties and continue till the present. The introduction to this method is presented and experimental experiences from NPI CAS and the collaboration are shared.

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32

Balabanski, Dimiter L. "Nuclear astrophysics studies with γ-ray beams: What do we expect to learn from them?" EPJ Web of Conferences 275 (2023): 01002. http://dx.doi.org/10.1051/epjconf/202327501002.

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An overview of the main directions of present-day studies with quasimonochromatic γ beams is discussed with an emphasis on the research opportunities which will be offered at the Extreme Light Infrastructure Nuclear Physics (ELI-NP) facility at Magurele near Bucharest in Romania. Experiments with γ beams at the extremes of high temperatures are outlined, with an emphasis on prospective studies related to nuclear astrophysics and astroparticle physics. Some of the experimental setups for nuclear structure, reaction, and astrophysics studies, which are available at ELI-NP, are described.

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33

Musumarra, Agatino. "From nuclear astrophysics to fundamental nuclear physics: challenging experimental approaches at n_TOF (CERN)." EPJ Web of Conferences 252 (2021): 05002. http://dx.doi.org/10.1051/epjconf/202125205002.

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The n_TOF installation at CERN is one of the leading neutron facilities worldwide undergoing a major update of the neutron spallation source. The update will provide improved n-TOF resolution in the experimental areas and the possibility to perform neutron cross section measurements at very high neutron flux (NEAR-Station). The renewed capabilities of the facility must be supported by smart and non-conventional experimental approaches. In this framework two examples will be reported. The first one concerns the measurement of a key reaction channel involved in Primordial Nucleosynthesis: the 7Be(n, α), by using a radioactive 7Be target. The second one provides a state-of-the-art scenario for the n-n scattering length measurement. This will be performed by neutron-deuteron (n-d) breakup three-body reaction. In this case, the envisaged experimental setup will provide a complete three-body kinematic reconstruction. By these important physics cases we are crossing the technological frontiers for charged particle and neutron detection.

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Kubono, Shigeru. "Experimental Challenge to Heavy Element Synthesis under Explosive Burning on Neutron Stars." EPJ Web of Conferences 227 (2020): 01010. http://dx.doi.org/10.1051/epjconf/202022701010.

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Binary stellar systems that involve a neutron star or two neutron stars make interesting phenomena, X-ray bursts and kilo-novae, respectively, which involve explosive burning either in the proton-rich environment or in the neutron-rich environment. These are very important problems for nuclear astrophysics. First, the current effort for the explosive hydrogen burning, the rapid proton capture (rp) process which would take place on a neutron star surface in X-ray burst is discussed together with a new X-ray observation that suggests the rp-process termination at around A = 100. The observation of the afterglow of the binary neutron star merger appears to be the kilo-nova predicted in the last decade in nuclear astrophysics, and to be the great success of the field. However, the detailed study of the kilo-nova by the r-process should be a great challenge for full understanding heavy element synthesis and the neutron star merger. Nuclear physics problems are discussed for the kilonova.

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35

Yamaguchi, H., S. Hayakawa, N. R. Ma, H. Shimizu, K. Okawa, L. Yang, D. Kahl, et al. "Experimental studies on astrophysical reactions at the low-energy RI beam separator CRIB." EPJ Web of Conferences 260 (2022): 03003. http://dx.doi.org/10.1051/epjconf/202226003003.

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Experimental studies on astrophysical reactions involving radioactive isotopes (RI) often accompany technical challenges. Studies on such nuclear reactions have been conducted at the low-energy RI beam separator CRIB, operated by Center for Nuclear Study, the University of Tokyo. We discuss two cases of astrophysical reaction studies at CRIB; one is for the 7Be+n reactions which may affect the primordial 7Li abundance in the Big-Bang nucleosynthesis, and the other is for the 22Mg(α, p) reaction relevantin X-raybursts.

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36

Piatti, Denise. "Underground measurement at LUNA found no evidence for a low-energy resonance in the ⁶Li(p, γ)⁷Be reaction." EPJ Web of Conferences 260 (2022): 11027. http://dx.doi.org/10.1051/epjconf/202226011027.

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The 6Li(p,γ)7Be reaction is involved in all three main nucleosynthesis scenarios: Big Bang Nucleosynthesis, the interaction of cosmic rays with interstellar matter, and stellar nucleosynthesis. Conflicting experimental results have been reported in literature for the 6Li(p,γ)7Be reaction cross section trend at astrophysical energies. A recent direct measurement found a resonance-like structure at Ec.m. = 195 keV, corresponding to an excited state at Ex ~ 5800 keV in 7Be which, however, has not been confirmed by either theoretical calculations or other direct measurements. In order to clarify the existence of this resonance, a new experiment was performed at the Laboratory for Underground Nuclear Astrophysics, located deep underground at Laboratori Nazionali del Gran Sasso (Italy). The 6Li(p,γ)7Be cross section was measured in the energy range Ec.m. = 60-350 keV with unprecedented sensitivity and no evidence for the alleged resonance was found.

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37

Cavanna, Francesca. "Nuclear astrophysics at Gran Sasso Laboratory: the LUNA experiment." EPJ Web of Conferences 178 (2018): 01007. http://dx.doi.org/10.1051/epjconf/201817801007.

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LUNA is an experimental approach for the study of nuclear fusion reactions based on an underground accelerator laboratory. Aim of the experiment is the direct measurement of the cross section of nuclear reactions relevant for stellar and primordial nucleosynthesis. In the following the latest results and the future goals will be presented.

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38

Chen, S. Z., S. W. Xu, J. J. He, J. Hu, C. E. Rolfs, N. T. Zhang, S. B. Ma, et al. "A new experimental setup established for low-energy nuclear astrophysics studies." Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment 735 (January 2014): 466–70. http://dx.doi.org/10.1016/j.nima.2013.10.015.

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39

Balantekin, A. B., J. Carlson, D. J. Dean, G. M. Fuller, R. J. Furnstahl, M. Hjorth-Jensen, R. V. F. Janssens, et al. "Nuclear theory and science of the facility for rare isotope beams." Modern Physics Letters A 29, no. 11 (April 7, 2014): 1430010. http://dx.doi.org/10.1142/s0217732314300109.

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The Facility for Rare Isotope Beams (FRIB) will be a world-leading laboratory for the study of nuclear structure, reactions and astrophysics. Experiments with intense beams of rare isotopes produced at FRIB will guide us toward a comprehensive description of nuclei, elucidate the origin of the elements in the cosmos, help provide an understanding of matter in neutron stars and establish the scientific foundation for innovative applications of nuclear science to society. FRIB will be essential for gaining access to key regions of the nuclear chart, where the measured nuclear properties will challenge established concepts, and highlight shortcomings and needed modifications to current theory. Conversely, nuclear theory will play a critical role in providing the intellectual framework for the science at FRIB, and will provide invaluable guidance to FRIB's experimental programs. This review overviews the broad scope of the FRIB theory effort, which reaches beyond the traditional fields of nuclear structure and reactions, and nuclear astrophysics, to explore exciting interdisciplinary boundaries with other areas.

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Kubono, Shigeru. "Experimental determination of astrophysical reaction rates with radioactive nuclear beams." Nuclear Physics A 693, no. 1-2 (October 2001): 221–48. http://dx.doi.org/10.1016/s0375-9474(01)01140-x.

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41

Mascali, David, Maurizio Busso, Alberto Mengoni, Simone Amaducci, Castro Giuseppe, Luigi Celona, Gianluigi Cosentino, et al. "The PANDORA project: an experimental setup for measuring in-plasma β-decays of astrophysical interest." EPJ Web of Conferences 227 (2020): 01013. http://dx.doi.org/10.1051/epjconf/202022701013.

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Experiments performed on Storage Rings have shown that lifetimes of beta-radionuclides can change dramatically as a function of theionization state. PANDORA (Plasmas for Astrophysics, Nuclear Decay Observation and Radiation for Archaeometry) aims at measuring, for the first time, nuclear β-decay rates in stellar-like conditions, especially for radionuclides involved in nuclear-astrophysics processes (BBN, s- processing, CosmoChronometers, Early Solar System formation). Compact magnetic plasma traps, where plasmas reach density ne~10n-1014 cm-3, and temperature Te~0.1-30 keV, are suitable for such studies. The decay rates can be measured as a function of the charge state distribution of the inplasma ions. The collaboration is now designing the plasma trap able to reach the needed plasma densities, temperatures and charge states distributions. A first list of radioisotopes, including tens of physics cases of potential interest is now available. Possible physics cases include, among the others, 2°4Tl, 63Ni, 6°Co, 171Tm, 147Pm, 85Kr, 176Lu and the pairs 187Re-187Os and 87Sr-87Rb, which play a crucial role as cosmo-clock. Physics cases are now under evaluation in terms of lifetime measurements feasibility in a plasma trap.

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ALT, E. O., B. F. IRGAZIEV, and A. M. MUKHAMEDZHANOV. "THREE-BODY COULOMB FINAL-STATE INTERACTION EFFECTS IN THE COULOMB BREAKUP OF LIGHT NUCLEI." Modern Physics Letters A 20, no. 13 (April 30, 2005): 947–63. http://dx.doi.org/10.1142/s0217732305017378.

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Coulomb breakup of a projectile in the Coulomb field of a fully stripped heavy nucleus is at present one of the most popular experimental methods to obtain information on reactions of interest in nuclear astrophysics. Its theoretical interpretation presents, however, considerable difficulties, due to the three-body nature and the infinite range of the Coulomb forces involved. Among the uncertainties affecting present analyses, the possible modification of the dissociation cross-section by three-body Coulomb final-state interactions plays a major role. Various methods which have been proposed to deal with it are briefly reviewed. However, none of them is based on a consistent and mathematically satisfactory quantum mechanical treatment, with the exception of the one proposed recently. The latter, being based on the prior form of the dissociation amplitude, makes use of a genuine three-charged particle wave function for the final state which is an exact solution of the three-body Schrödinger equation, albeit only asymptotically, i.e. for large distances. Nevertheless, interesting conclusion can be drawn concerning the influence of three-body Coulomb final-state interactions on quantities of astrophysical interest.

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Graber, Vanessa, Nils Andersson, and Michael Hogg. "Neutron stars in the laboratory." International Journal of Modern Physics D 26, no. 08 (April 6, 2017): 1730015. http://dx.doi.org/10.1142/s0218271817300154.

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Neutron stars are astrophysical laboratories of many extremes of physics. Their rich phenomenology provides insights into the state and composition of matter at densities which cannot be reached in terrestrial experiments. Since the core of a mature neutron star is expected to be dominated by superfluid and superconducting components, observations also probe the dynamics of large-scale quantum condensates. The testing and understanding of the relevant theory tend to focus on the interface between the astrophysics phenomenology and nuclear physics. The connections with low-temperature experiments tend to be ignored. However, there has been dramatic progress in understanding laboratory condensates (from the different phases of superfluid helium to the entire range of superconductors and cold atom condensates). In this review, we provide an overview of these developments, compare and contrast the mathematical descriptions of laboratory condensates and neutron stars and summarize the current experimental state-of-the-art. This discussion suggests novel ways that we may make progress in understanding neutron star physics using low-temperature laboratory experiments.

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Navrátil, Petr. "ARIEL experiments and theory." Journal of Physics: Conference Series 2391, no. 1 (December 1, 2022): 012002. http://dx.doi.org/10.1088/1742-6596/2391/1/012002.

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Abstract I present an overview of experiments at TRIUMF ARIEL and ISAC facilities covering both the current and the future envisioned programs. I also briefly review theory program at TRIUMF that relates to the ARIEL experimental program. I highlight several recent experimental results from the nuclear astrophysics, nuclear structure, fundamental symmetries, and the sterile neutrino search. Finally, I mention ongoing theoretical ab initio calculations of the proton capture on 7Li related to the X17 boson observation.

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Massimi, Cristian. "Nuclear astrophysics activities at the n_TOF facility at CERN." EPJ Web of Conferences 275 (2023): 01009. http://dx.doi.org/10.1051/epjconf/202327501009.

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The n_TOF facility at CERN is operational since 2001, and provides neutron-induced cross section data of interest to several research fields, including nuclear astrophysics. The neutron time-of-flight (TOF) facility features three experimental areas located at different distances from the pulsed neutron source. Two beam lines at nominal distance of 185 and 19 m are especially equipped for TOF experiments. A third station at approximately 3 meters from the neutron source was conceived for irradiation and activation measurements. So far, neutron-induced cross sections for more than 100 isotopes have been measured.

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Arnould, M. "Nuclear reactions in astrophysics: recent experimental and theoretical studies, and further quests." Nuclear Physics A 538 (March 1992): 493–503. http://dx.doi.org/10.1016/0375-9474(92)90798-o.

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Liu, Weiping, Zhihong Li, Jianjun He, Xiaodong Tang, Gang Lian, Jun Su, Yangping Shen, et al. "Commissioning of Underground Nuclear Astrophysics Experiment JUNA in China." EPJ Web of Conferences 260 (2022): 08001. http://dx.doi.org/10.1051/epjconf/202226008001.

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Underground Nuclear Astrophysics Experiment in China (JUNA) has been commissioned by taking the advantage of the ultra-low background in Jinping underground lab. High current mA level 400 KV accelerator with an ECR source and BGO detectors were commissioned. JUNA studies directly a number of nuclear reactions important to hydrostatic stellar evolution at their relevant stellar energies. In the first quarter of 2021, JUNA performed the direct measurements of 25Mg(p,γ)26Al, 19F(p,α)16O, 13C(α,n)16O and 12C(α,γ)16O near the Gamow window. The experimental results reflect the potential of JUNA with higher statistics, precision and sensitivity of the data. The preliminary results of JUNA experiment and future plan are given.

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GROHMANN, M., C. A. Z. VASCONCELLOS, G. F. MARRANGHELLO, and F. FERNÁNDEZ. "HEAVY-ION AND ASTROPHYSICS CONSTRAINTS IN THE PARAMETRIC COUPLING MODEL." International Journal of Modern Physics D 19, no. 08n10 (August 2010): 1667–72. http://dx.doi.org/10.1142/s0218271810017950.

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The relativistic parametric coupling model is used here to describe global static properties of nuclear matter and neutron stars. Using recent observational data related to neutron star properties and experimental results of heavy-ion collisions, we review some properties of the effective model and we impose this way new constraints on its coupling constants. Then we analyze the consequences on already known parameters of nuclear matter, i.e., the compression modulus, the effective nucleon mass and the maximum neutron star mass predicted by integrating the Tolman–Oppenheimer–Volkoff equations. We make use of recent data on flow analysis to constrain the parameters of the theory and to achieve this goal, and have explored the parametric coupling model in a wide range of parameters. Our predictions for the compression modulus of nuclear matter and for the maximum mass of neutron stars are in good agreement with the observational data.

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Tursunmakhatov, K. I., R. Yarmukhamedov, and S. B. Igamov. "Asymptotic normalization coefficient for α+d →6Li from the peripheral direct capture d(α,γ)6 reaction and the astrophysical S factor at Big Bang energies." EPJ Web of Conferences 227 (2020): 02016. http://dx.doi.org/10.1051/epjconf/202022702016.

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The results of the analysis of the new experimental astrophysical S factors Sexp24(E) [D. Trezzi, et al., Astropart. Phys. 89, 57 (2017)] and those measured earlier [R. G. Robertson, et al., Phys. Rev. Lett. 47, 1867 (1981)] for the nuclear-astrophysical d(α,γ)6Li reaction directly measured at extremely low energies E, are presented. New estimates and their uncertainties have been obtained for values of the asymptotic normalization coefficient for α + γ → 6Li and for the direct astrophysical S factors at Big Bang energies.

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Yadav, Chandrabhan, and Moshe Friedman. "Novel experimental techniques for neutron induced charge particle reaction studies in nuclear astrophysics." EPJ Web of Conferences 260 (2022): 11048. http://dx.doi.org/10.1051/epjconf/202226011048.

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Neutron induced reaction studies on various unstable and short-lived nuclei play a very important role in understanding the various nucleosynthesis processes occuring in astrophysics scenario. We discuss here our approach to study neutron induced charge particle cross-section for various unstable and short-lived nuclei at effective temperatures of ~1.5-3.5 GK using the 7Li(p, n) reaction as a neutron source with ﬁve orders of magnitude higher neutron intensities with respect to currently available neutron time-of-ﬂight facilities, using SARAF accelarator and Liquid Lithium Target (LiLiT) facility.

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