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Artículos de revistas sobre el tema "Nuclear astrophysic"

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Autor: Grafiati

Publicado: 11 de marzo de 2023

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1

Gyürky, György. "Challenges and Requirements in High-Precision Nuclear Astrophysics Experiments". Universe 8, n.º 4 (28 de marzo de 2022): 216. http://dx.doi.org/10.3390/universe8040216.

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In the 21th century astronomical observations, as well as astrophysical models, have become impressively precise. For a better understanding of the processes in stellar interiors, the nuclear physics of astrophysical relevance—known as nuclear astrophysics—must aim for similar precision, as such precision is not reached yet in many cases. This concerns both nuclear theory and experiment. In this paper, nuclear astrophysics experiments are put in focus. Through the example of various parameters playing a role in nuclear reaction studies, the difficulties of reaching high precision and the possible solutions are discussed.

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2

Depalo, Rosanna. "Nuclear Astrophysics Deep Underground". International Journal of Modern Physics: Conference Series 46 (enero de 2018): 1860003. http://dx.doi.org/10.1142/s2010194518600030.

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Cross sections of nuclear reactions relevant for astrophysics are crucial ingredients to understand the energy generation inside stars and the synthesis of the elements. At astrophysical energies, nuclear cross sections are often too small to be measured in laboratories on the Earth surface, where the signal would be overwhelmed by the cosmic-ray induced background. LUNA is a unique Nuclear Astrophysics experiment located at Gran Sasso National Laboratories. The extremely low background achieved at LUNA allows to measure nuclear cross sections directly at the energies of astrophysical interest. Over the years, many crucial reactions involved in stellar hydrogen burning as well as Big Bang nucleosynthesis have been measured at LUNA. The present contribution provides an overview on underground Nuclear Astrophysics as well as the latest results and future perspectives of the LUNA experiment.

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3

Adsley, Philip. "Transfer Reactions in Nuclear Astrophysics". EPJ Web of Conferences 275 (2023): 01001. http://dx.doi.org/10.1051/epjconf/202327501001.

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Transfer reactions are important tool in nuclear astrophysics. These reactions allow us to identify states in nuclei and to find the corresponding energies, to determine if these states can contribute to astrophysical nuclear reactions and ultimately to determine the strength of that contribution. In this paper,the basic details of how transfer reactions may be used in nuclear astrophysics are set out along with some common pitfalls to avoid.

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4

Descouvemont, P. "Astrophysica for Windows: a PC software for nuclear astrophysics". Nuclear Physics A 688, n.º 1-2 (mayo de 2001): 557–59. http://dx.doi.org/10.1016/s0375-9474(01)00786-2.

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5

Lépine-Szily, Alinka y Pierre Descouvemont. "Nuclear astrophysics: nucleosynthesis in the Universe". International Journal of Astrobiology 11, n.º 4 (9 de mayo de 2012): 243–50. http://dx.doi.org/10.1017/s1473550412000158.

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AbstractNuclear astrophysics is a relatively young science; it is about half a century old. It is a multidisciplinary subject, since it combines nuclear physics with astrophysics and observations in astronomy. It also addresses fundamental issues in astrobiology through the formation of elements, in particular those required for a carbon-based life. In this paper, a rapid overview of nucleosynthesis is given, mainly from the point of view of nuclear physics. A short historical introduction is followed by the definition of the relevant nuclear parameters, such as nuclear reaction cross sections, astrophysical S-factors, the energy range defined by the Gamow peak and reaction rates. The different astrophysical scenarios that are the sites of nucleosynthesis, and different processes, cycles and chains that are responsible for the building of complex nuclei from the elementary hydrogen nuclei are then briefly described.

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6

RAUSCHER, THOMAS. "THE PATH TO IMPROVED REACTION RATES FOR ASTROPHYSICS". International Journal of Modern Physics E 20, n.º 05 (mayo de 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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7

Broggini, Carlo. "Origin and status of LUNA at Gran Sasso". Modern Physics Letters A 29, n.º 34 (6 de noviembre de 2014): 1430038. http://dx.doi.org/10.1142/s0217732314300389.

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The ultimate goal of nuclear astrophysics, the union of nuclear physics and astronomy, is to provide a comprehensive picture of the nuclear reactions which power the stars and, in doing so, synthesize the chemical elements. Deep underground in the Gran Sasso Laboratory the key reactions of the proton–proton chain and of the carbon–nitrogen–oxygen cycle have been studied down to the energies of astrophysical interest. The main results obtained in the past 20 years are reviewed and their influence on our understanding of the properties of the neutrino, the Sun, and the Universe itself is discussed. Finally, future developments of underground nuclear astrophysics beyond the study of hydrogen burning are outlined.

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8

Shen, Yang-Ping, Bing Guo y Wei-Ping Liu. "An indirect technique in nuclear astrophysics: alpha-cluster transfer reaction". EPJ Web of Conferences 260 (2022): 01001. http://dx.doi.org/10.1051/epjconf/202226001001.

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Helium(4He, or α)is the second most abundant element in the observable Universe. The α-particle induced reactions such as(α, γ), (α, n) and (α, p) play a crucial role in nuclear astrophysics, especially for understanding stellar heliumburning. Because of the strong Coulomb repulsion, it is greatly hindered to directly measure the cross sections for these α-capture reactions at stellar energies. Alpha-cluster transfer reaction is a powerful tool for investigation of astrophysical(α, γ), (α, n)and(α, p)reactions since it can preferentially populate the natural-parity states with an α-cluster structure which dominantly contribute to these astrophysical α-capture reactions during stellar heliumburning. In this paper, we reviewthe theoretical scheme, theexperimental technique, astrophysical applications and the future perspectives of such approach based on α-cluster transfer reactions.

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9

CHAMPAGNE, A. E. y C. ILIADIS. "FIRST RESULTS FROM LENA". Modern Physics Letters A 22, n.º 04 (10 de febrero de 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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10

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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11

Arnould, M. y K. Takahashi. "Nuclear astrophysics". Reports on Progress in Physics 62, n.º 3 (1 de enero de 1999): 395–462. http://dx.doi.org/10.1088/0034-4885/62/3/003.

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12

Penionzhkevich, Yu E. "Nuclear astrophysics". Physics of Atomic Nuclei 73, n.º 8 (agosto de 2010): 1460–68. http://dx.doi.org/10.1134/s106377881008020x.

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13

Langanke, K. "Nuclear astrophysics". Nuclear Physics A 654, n.º 1-2 (julio de 1999): C330—C349. http://dx.doi.org/10.1016/s0375-9474(99)00262-6.

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14

Rauscher, Thomas y Friedrich-Karl Thielemann. "Nuclear astrophysics". Europhysics News 32, n.º 6 (noviembre de 2001): 224–26. http://dx.doi.org/10.1051/epn:2001608.

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15

Haxton, W. C. "Nuclear astrophysics". Nuclear Physics A 553 (marzo de 1993): 397–406. http://dx.doi.org/10.1016/0375-9474(93)90638-e.

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16

Buompane, Raffaele, Antonino Di Leva, Lucio Gialanella, Gianluca Imbriani, Lizeth Morales-Gallegos y Mauro Romoli. "Recent Achievements of the ERNA Collaboration". Universe 8, n.º 2 (21 de febrero de 2022): 135. http://dx.doi.org/10.3390/universe8020135.

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For more than two decades, the ERNA collaboration has investigated nuclear processes of astrophysical interest through the direct measurement of cross sections or the identification of the nucleosynthesis effects. Measurements of cross-section, reported in this publication, of radiative capture reactions have been mainly conducted using the ERNA Recoil Mass Separator, and more recently with an array of charged particle detector telescopes designed for nuclear astrophysics measurements. Some results achieved with ERNA will be reviewed, with a focus on the results most relevant for nucleosynthesis in AGB and advanced burning phases.

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17

SARRIGUREN, P., R. ÁLVAREZ-RODRÍGUEZ, O. MORENO y E. MOYA DE GUERRA. "THE GAMOW-TELLER RESPONSE IN DEFORMED NUCLEI". International Journal of Modern Physics E 15, n.º 07 (octubre de 2006): 1397–406. http://dx.doi.org/10.1142/s0218301306004958.

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We study Gamow-Teller strength distributions within a QRPA approach performed on top of a deformed Skyrme-Hartree-Fock+BCS single particle basis with the inclusion of residual spin-isospin interactions in both particle-hole and particle-particle channels. We focus our attention in several problems of interest in Nuclear Structure and Nuclear Astrophysics, such as the β-decay properties of proton-rich medium-mass nuclei of astrophysical interest and the deformation dependence of the Gamow-Teller strength distributions in neutron deficient Pb isotopes. We also discuss the role of deformation in the two-neutrino double beta decay.

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18

XU, RENXIN. "ASTRO-QUARK MATTER: A CHALLENGE FACING ASTROPARTICLE PHYSICS". Modern Physics Letters A 23, n.º 17n20 (28 de junio de 2008): 1629–42. http://dx.doi.org/10.1142/s021773230802803x.

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Quark matter both in terrestrial experiment and in astrophysics is briefly reviewed. Astrophysical quark matter could appear in the early Universe, in compact stars, and as cosmic rays. Emphasis is put on quark star as the nature of pulsars. Possible astrophysical implications of experiment-discovered sQGP are also concisely discussed.

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19

Frebel, Anna. "From Nuclei to the Cosmos: Tracing Heavy-Element Production with the Oldest Stars". Annual Review of Nuclear and Particle Science 68, n.º 1 (19 de octubre de 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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20

Murase, Kohta y Imre Bartos. "High-Energy Multimessenger Transient Astrophysics". Annual Review of Nuclear and Particle Science 69, n.º 1 (19 de octubre de 2019): 477–506. http://dx.doi.org/10.1146/annurev-nucl-101918-023510.

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The recent discoveries of high-energy cosmic neutrinos and gravitational waves from astrophysical objects have led to a new era of multimessenger astrophysics. In particular, electromagnetic follow-up observations triggered by these cosmic signals have proved to be highly successful and have brought about new opportunities in time-domain astronomy. We review high-energy particle production in various classes of astrophysical transient phenomena related to black holes and neutron stars, and discuss how high-energy emission can be used to reveal the underlying physics of neutrino and gravitational-wave sources.

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21

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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22

Kubono, S. "Nuclear Astrophysics with Radioactive Nuclear Beams". Progress of Theoretical Physics 96, n.º 2 (1 de agosto de 1996): 275–306. http://dx.doi.org/10.1143/ptp.96.275.

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23

APRAHAMIAN, A., K. LANGANKE y M. WIESCHER. "Nuclear structure aspects in nuclear astrophysics". Progress in Particle and Nuclear Physics 54, n.º 2 (abril de 2005): 535–613. http://dx.doi.org/10.1016/j.ppnp.2004.09.002.

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24

Arcones, Almudena, Dan W. Bardayan, Timothy C. Beers, Lee A. Bernstein, Jeffrey C. Blackmon, Bronson Messer, B. Alex Brown et al. "White paper on nuclear astrophysics and low energy nuclear physics Part 1: Nuclear astrophysics". Progress in Particle and Nuclear Physics 94 (mayo de 2017): 1–67. http://dx.doi.org/10.1016/j.ppnp.2016.12.003.

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25

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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26

Cavanna, Francesca y Paolo Prati. "Direct measurement of nuclear cross-section of astrophysical interest: Results and perspectives". International Journal of Modern Physics A 33, n.º 09 (30 de marzo de 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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27

Käppeler, F. "Astrophysics at nuclear reactors". Acta Physica Hungarica 75, n.º 1-4 (diciembre de 1994): 41–45. http://dx.doi.org/10.1007/bf03156556.

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28

Salpeter, Edwin E. "Nuclear Astrophysics Before 1957". Publications of the Astronomical Society of Australia 25, n.º 1 (2008): 1–6. http://dx.doi.org/10.1071/as07036.

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AbstractI discuss especially my summer with Willy Fowler at Kellogg Radiation Laboratory in 1951, where I did my ‘triple alpha’ work. I also go back even earlier to Arthur Eddington and Hans Bethe. The 1953 summer school in Ann Arbor only gets a mention.

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29

Gialanella, Lucio, Antonino Di Leva y Fillipo Terrasi. "Nuclear Astrophysics at CIRCE". Nuclear Physics News 28, n.º 3 (3 de julio de 2018): 20–24. http://dx.doi.org/10.1080/10619127.2018.1463018.

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30

Huang, Meirong, Hernan J. Quevedo, Guoqiang Zhang y Aldo Bonasera. "Nuclear Astrophysics with Lasers". Nuclear Physics News 29, n.º 3 (3 de julio de 2019): 9–13. http://dx.doi.org/10.1080/10619127.2019.1603555.

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31

Broggini, Carlo. "Nuclear Astrophysics with LUNA". Journal of Physics: Conference Series 703 (abril de 2016): 012006. http://dx.doi.org/10.1088/1742-6596/703/1/012006.

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32

Malaney, Robert A. "Supercomputers And Nuclear Astrophysics". Computers in Physics 2, n.º 6 (1988): 40. http://dx.doi.org/10.1063/1.4822797.

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33

Dillmann, I. y R. Reifarth. "Nuclear astrophysics with neutrons". Journal of Instrumentation 7, n.º 04 (19 de abril de 2012): C04014. http://dx.doi.org/10.1088/1748-0221/7/04/c04014.

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34

Jonson, B. "Nuclear processes in astrophysics". Physica Scripta T59 (1 de enero de 1995): 53–58. http://dx.doi.org/10.1088/0031-8949/1995/t59/006.

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35

Schatz, Hendrik. "Trends in nuclear astrophysics". Journal of Physics G: Nuclear and Particle Physics 43, n.º 6 (16 de mayo de 2016): 064001. http://dx.doi.org/10.1088/0954-3899/43/6/064001.

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36

Bertulani, C. A. y T. Kajino. "Frontiers in nuclear astrophysics". Progress in Particle and Nuclear Physics 89 (julio de 2016): 56–100. http://dx.doi.org/10.1016/j.ppnp.2016.04.001.

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37

Mohr, P., T. Rauscher, K. Sonnabend, K. Vogt y A. Zilges. "Photoreactions in nuclear astrophysics". Nuclear Physics A 718 (mayo de 2003): 243–46. http://dx.doi.org/10.1016/s0375-9474(03)00721-8.

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38

Smith, Michael S. "Nuclear data for astrophysics". Nuclear Physics A 718 (mayo de 2003): 339–46. http://dx.doi.org/10.1016/s0375-9474(03)00736-x.

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39

Schatz, H. "Nuclear masses in astrophysics". International Journal of Mass Spectrometry 349-350 (septiembre de 2013): 181–86. http://dx.doi.org/10.1016/j.ijms.2013.03.016.

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40

Rehm, K. E. "Experiments in Nuclear Astrophysics". Nuclear Physics A 787, n.º 1-4 (mayo de 2007): 289–98. http://dx.doi.org/10.1016/j.nuclphysa.2006.12.045.

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41

Mathews, Grant J. "Frontiers of Nuclear Astrophysics". Nuclear Physics A 805, n.º 1-4 (junio de 2008): 303c—312c. http://dx.doi.org/10.1016/j.nuclphysa.2008.02.258.

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42

Buchmann, L., P. Amaudruz, J. D'Auria, D. Hutcheon, C. Matei, J. Pearson, C. Ruiz et al. "Nuclear Astrophysics at TRIUMF". Nuclear Physics A 805, n.º 1-4 (junio de 2008): 462c—469c. http://dx.doi.org/10.1016/j.nuclphysa.2008.02.267.

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43

Kubono, S., Dam N. Binh, S. Hayakawa, H. Hashimoto, D. Kahl, Y. Wakabayashi, H. Yamaguchi et al. "Nuclear Clusters in Astrophysics". Nuclear Physics A 834, n.º 1-4 (marzo de 2010): 647c—650c. http://dx.doi.org/10.1016/j.nuclphysa.2010.01.113.

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44

Matteson, J. L. "The nuclear astrophysics explorer". Advances in Space Research 11, n.º 8 (enero de 1991): 369–78. http://dx.doi.org/10.1016/0273-1177(91)90190-u.

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45

Arnould, M. y M. Rayet. "Nuclear reactions in astrophysics". Annales de Physique 15, n.º 3 (1990): 183–254. http://dx.doi.org/10.1051/anphys:01990001503018300.

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46

Grawe, H., K. Langanke y G. Martínez-Pinedo. "Nuclear structure and astrophysics". Reports on Progress in Physics 70, n.º 9 (29 de agosto de 2007): 1525–82. http://dx.doi.org/10.1088/0034-4885/70/9/r02.

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47

Reifarth, R., S. Dababneh, S. Fiebiger, J. Glorius, K. Göbel, M. Heil, P. Hillmann et al. "Nuclear astrophysics at FRANZ". Journal of Physics: Conference Series 940 (enero de 2018): 012024. http://dx.doi.org/10.1088/1742-6596/940/1/012024.

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48

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, n.º 04 (mayo de 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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DUBOVICHENKO, SERGEY, ALBERT DZHAZAIROV-KAKHRAMANOV y NADEZHDA AFANASYEVA. "RADIATIVE NEUTRON CAPTURE ON 9Be, 14C, 14N, 15N AND 16O AT THERMAL AND ASTROPHYSICAL ENERGIES". International Journal of Modern Physics E 22, n.º 10 (octubre de 2013): 1350075. http://dx.doi.org/10.1142/s0218301313500754.

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The total cross-sections of the radiative neutron capture processes on 9 Be , 14 C , 14 N , 15 N and 16 O are described in the framework of the modified potential cluster model with the classification of orbital states according to Young tableaux. The continued interest in the study of these reactions is due, on the one hand, to the important role played by this process in the analysis of many fundamental properties of nuclei and nuclear reactions, and, on the other hand, to the wide use of the capture cross-section data in the various applications of nuclear physics and nuclear astrophysics, and, also, to the importance of the analysis of primordial nucleosynthesis in the Universe. This article is devoted to the description of results for the processes of the radiative neutron capture on certain light atomic nuclei at thermal and astrophysical energies. The considered capture reactions are not part of stellar thermonuclear cycles, but involve in the reaction chains of inhomogeneous Big Bang models.

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50

Wang, Luohuan, Jun Su, Yangping Shen, Jianjun He, Liyong Zhang, Xinyue Li, Gang Lian et al. "Measurement of the ¹⁸O(α, γ)²²Ne resonances at JUNA". EPJ Web of Conferences 260 (2022): 11015. http://dx.doi.org/10.1051/epjconf/202226011015.

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22Ne(α,n)25Mg is one of the main neutron sources of the s process. 22Ne is produced by the 14N(α, γ)18F(β+)18O(α, γ)22Ne reaction chain in the helium burning, thus, the production rate of 22Ne is dominated by 14N(α,γ)18F and 18O(α,γ)22Ne. At the astrophysical relevant temperatures, the 18O(α,γ)22Ne reaction rates are determined by several low-energy resonances. In this work, the 18O(α,γ)22Ne reaction was measured at the 400 kV accelerator of Jinping Underground Nuclear Astrophysics experiment (JUNA). The γ-ray yields of the resonances between 470 to 770 keV were obtained.

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