Nuclear Astrophysics Research Research Articles

Vortex photon induced nuclear reaction: Mechanism, model, and application to the studies of giant resonance and astrophysical reaction rate

The vortex photon beam induced nuclear reaction is studied. The interaction formalism of nuclei with vortex photons is developed and incorporated into the statistical reaction model to calculate reaction cross-sections. For 138 nuclei of high nuclear astrophysics and structure interest, the cross-sections of γ-ray emission and neutron production from the decay of the giant resonances (GR) populated by vortex photons, e.g., (γvo,γemit) and (γvo,nprod.), are computed. It is shown that for the (γvo,γemit) and (γvo,nprod.) cross-sections, the GR contribution of an individual L is either enhanced or suppressed depending on the parameters of vortex γ-rays, and the contribution from the GR of a specific L can be identified and deduced. To this end, a novel method to exclusively determine the γ-strength function (γSF) for the GR of a specific L is proposed considering the (γvo,γemit) and (γvo,nprod.) measurements, and the feasibility studies demonstrate that the γSF for the giant quadrupole resonance can be extracted. Furthermore, the astrophysical reaction rates of the vortex photon induced reactions in p-process are investigated. It is indicated that photo-nuclear reactions induced by vortex photons will bring new insights in nuclear physics and astrophysics research.

Understanding radioactive ion beam production at ISAC through yield measurements and simulations

The high-intensity proton beam of the TRIUMF 500 MeV cyclotron offers unique opportunities to produce rare isotopes by irradiating a variety of targets. In particular, the ISAC (Isotope Separation and ACceleration) facility provides the infrastructure to deliver customized rare ion beams for fundamental research in nuclear physics, astrophysics, material science, and nuclear medicine. A continuous effort is made to develop new radioactive ion beams (RIB) and improve their intensity or purity, properties that depend strongly on the type of target, operating conditions, the ion source, and beam transport efficiency. Yield data and theoretical production rates based on FLUKA and Geant4 simulations are collected in the TRIUMF Isotope Database, providing a valuable resource for RIB development and experiment planning. This paper introduces the newly upgraded TRIUMF Isotope Database and presents examples on how its resources can be used to plan experiments and understand the origin of certain RIB. In particular we discuss the collection of 155Tb which is an important component of medical isotope research at TRIUMF.

Recovery of no-carrier-added 41Ca, 44Ti, and 26Al from high-energy proton-irradiated vanadium targets

Abstract Many useful and needed radionuclides for medicinal, astrophysical, and environmental research are produced naturally in inefficient quantities or not-at-all. In the method described here, rare cosmogenic isotopes were produced via spallation reactions in metallic vanadium and separated without adding any carriers. In the SINQ facility at the Paul Scherrer Institut, the vanadium targets were irradiated for two years with high-energy protons (≤590 MeV). After a cooling period of eight years, only relatively long-lived radionuclides such as 32Si, 44Ti, 41Ca, and 26Al remain present. After target dissolution, 32Si was first separated for a prospective half-life redetermination. The remaining 32Si-free solution was used for extracting 44Ti, 41Ca, and 26Al, three key isotopes which are scientifically interesting for nuclear astrophysics research as well as medical applications. Each separation scheme employed ion-exchange and extraction chromatography; developed and optimized using inactive model solutions analyzed with Inductively Coupled Plasma–Optical Emission Spectrometry (ICP–OES). The irradiated samples were tracked with γ-ray spectroscopy for γ-ray emitting impurities. As a result, radiochemically pure sample solutions of 44Ti, 41Ca, and 26Al were obtained as “ready for use” in different application fields.

Background gamma measurement for low energy astrophysical reaction at FRENA

The majority of astrophysical reactions have very low cross-sections (nanobarn to picobarn range) and significant error bars [1, 2]. Hence γ-ray background studies up to 3 MeV have been performed inside the Facility for Research in Experimental Nuclear Astrophysics (FRENA), Saha Institute of Nuclear Physics, Kolkata, India. A meticulous background calculation has been performed at different positions inside the accelerator hall and beam hall using two NaI(Tl) detectors [3]. An XPS measurement has been carried out to identify elements present in the FRENA wall concrete. Activity calculations done in [4] shows that neutrons produced by various experiments may combine with any nearby elements and form various radioactive isotopes with long half-lives, which may produce a γ-ray background .

Study for the long-lived gamma background due to neutron emitting calibration reactions

In this article, a detailed theoretical investigation has been done on the long-lived gamma background due to neutron emitting reactions. It mainly focused on the experiments that will be used to calibrate energy with the terminal voltage of an upcoming Facility for Research in Experimental Nuclear Astrophysics (FRENA). Many reactions like (p, n), (p, γ) have been utilized in various accelerator facilities around the globe for energy calibration purposes. Neutron emitting reactions like 7Li(p, n), 13C(p, n), 19F(p, n), 27Al(p, n), etc. have been very commonly used. For such reactions, a significant number of neutrons produced from such experiments can interact with surrounding elements like copper, tantalum, stainless steel (SS304 and SS316), concrete materials,etc. These interactions may create long-lived gamma activity in the vicinity of the accelerator and detection area. Background gammas from these radioactive isotopes can interfere with gamma measurements in future experiments. The present study has been done to investigate those possibilities of gamma background which may occur due to the calibration study by neutron emitting experiments. Here 7Li(p, n), 13C(p, n), 19F(p, n) and 27Al(p, n) reactions having neutron threshold energies 1.8803, 3.2355, 4.2351, 5.8036 MeV respectively are chosen keeping in mind the proton energy available at the facility.

The preparation of isotopic boron targets – searching for a more consistent approach

The reliable availability of isotopic boron targets has gained in importance concerning light ion reactions withing the realm of nuclear astrophysics research and remain somewhat elusive. An exhaustive approach was undertaken via electron beam evaporation to produce self-supporting and backed targets spanning quite a few isotopic samples across several suppliers, resulting only in limited success. Details of the extensive sample preparation procedures undertaken, and the experimental deposition techniques explored will be presented.

Radiative Capture on Nuclear Isomers: Direct Measurement of the ^{26m}Al(p,γ)^{27}Si Reaction.

We present the first direct measurement of an astrophysical reaction using a radioactive beam of isomeric nuclei. In particular, we have measured the strength of the key 447-keV resonance in the ^{26m}Al(p,γ)^{27}Si reaction to be 432_{-226}^{+146} meV and find that this resonance dominates the thermally averaged reaction rate for temperatures between 0.3 and 2.5GK. This work represents a critical development in resolving one of the longest standing issues in nuclear astrophysics research, relating to the measurement of proton capture reactions on excited quantum levels, and offers unique insight into the destruction of isomeric ^{26}Al in astrophysical plasmas.

Capitalizing on nuclear data libraries’ comprehensiveness to obtain solar system r-process abundances

The recent observation of neutron stars merger by the laser interferometer gravitational-wave observatory collaboration and the measurements of the event’s electromagnetic spectrum as a function of time for different wavelengths have altered profoundly our understanding of the r-process site as well as considerably energized nuclear astrophysics research efforts. R-process abundances are a key element in r-process simulations, as a successful calculation must account for these abundances in the final debris of a stellar cataclysmic event. In this article, mankind’s complete knowledge of neutron cross sections obtained over the last 80 years, as encapsulated in the latest release of the evaluated nuclear data file (ENDF/B) library, is used to obtain solar system r-process abundances in a comprehensive data approach. ENDF/B cross sections have been successfully used for decades in nuclear power and defense applications and are now used to obtain r-process abundances in a fully traceable and documented way. This article r-process abundances provide complementary insights on the astrophysical events, overall quality of neutron capture data in the astrophysical region of temperatures, and demonstrate issues with the s-process contribution subtraction procedure.

Measurement and simulation of gamma-ray background in a low energy accelerator facility

The γ-ray background in the indoor environment has been measured up to 3 MeV to evaluate the feasibility of studying low cross-section (nanobarn to picobarn range) astrophysical reactions at the Facility for Research in Experimental Nuclear Astrophysics (FRENA), Saha Institute of Nuclear Physics, Kolkata. An n-type coaxial HPGe detector with 20% relative efficiency has been placed at different locations in the accelerator and beam halls for the measurement. The measured activity has been compared with that at two laboratories (with standard brick walls) with and without passive and active radiation shieldings. As the halls at FRENA are well shielded by concrete, the contribution of the shielding in indoor γ-ray background has been delineated by simulation using a 4π-geometry model.

Evolution of shell structure in exotic nuclei

The next generation of rare-isotope beam facilities will enable access to key regions of the nuclear chart, where the measured properties of short-lived isotopes will challenge our current theoretical picture and help develop a comprehensive model of the atomic nucleus. This article reviews the mechanisms driving the evolution of shell structure in exotic nuclei that impact nuclear physics and nuclear astrophysics research.

Nuclear astrophysics studies at NIPNE

I will present results of doing nuclear astrophysics research at the National Institute for Physics and Nuclear Engineering, Bucharest-Magurele in the last 2-3 years.Own Nuclear Astrophysics Group (NAG) is focused on the basic types of experiments:-Direct measurements at low and very low energies with ion or alpha beams from the local 3 MV tandetron accelerator. We concentrate on activation measurements. The use of the ultra-low background laboratory in a salt mine at Slanic-Prahova, about 120 km away and of a beta-gamma coincidence unit at home is providing competitive sensitivity.-Indirect measurements done with beams at international facilities with radioactive beams: TAMU and RIBF RIKEN.With help from colleagues, I will mention some theory advances, too.

A 50 kW Liquid-Lithium Target for BNCT and Material-Science Applications

A compact Liquid Lithium Target (LiLiT) has been operating at SARAF for several years with beam power of several kW (1.9-2.5 MeV, up to 2 mA). When bombarding the lithium with low energy protons neutrons are generated. The neutron source, mainly used for nuclear astrophysics research, was decommissioned in 2016 towards an upgraded model - with possible applications to Boron Neutron Capture Therapy (BNCT) and material-science studies. The improved version has been designed to sustain 50 kW proton beam power (2.5 MeV, ~20 mA) to provide sufficient neutron flux required for clinical BNCT application. The new model has a 50 mm wide lithium jet to enable dissipation of the higher beam power and an improved heat exchanger to remove the power to a secondary cooling loop. A new Annular Linear INduction electro-magnetic pump (ALIN) has been designed and built to provide the required lithium flow rate. Other mechanical improvements facilitate the maintenance of the system and the robustness of operation. Radiological risks due to the 7Be produced in the reaction are reduced by using an integrated lead shielding of the lithium reservoir. An integrated neutron moderator is being designed to adjust the neutron energy to the spectrum best suited to BNCT. A low power (6 kW) model of the new design with a narrower nozzle (18 mm wide) and a rotating-magnet electro-magnetic pump is operating at SARAF to support the ongoing astrophysics and nuclear research program [1], [2]. To fulfill clinical BNCT, the upgraded LiLiT model will require an accelerator of appropriate energy and intensity. The design features of the new system are presented in this paper.

Multidiagnostics setups for magnetoplasmas devoted to astrophysics and nuclear astrophysics research in compact traps

Magnetized plasmas in compact trap may become experimental environments for the investigation of nuclear β-decays of astrophysical interest. In the framework of the project PANDORA (Plasmas for Astrophysics, Nuclear Decays Observation and Radiation for Archaeometry) the research activities are devoted to demonstrate the feasibility of an experiment aiming at correlating radionuclides lifetimes to the in-plasma ions charge state distribution (CSD). The paper describes the multidiagnostics setup now available at INFN-LNS, which allows unprecedented investigations of magnetoplasma properties in terms of density, temperature and CSD. The developed setup includes an interfero-polarimeter for total plasma density measurements, a multi-X-ray detectors system for X-ray spectroscopy (including time resolved spectroscopy), a X-ray pin-hole camera for high-resolution 2D space resolved spectroscopy and different spectrometers for the plasma-emitted visible light characterization. A description of recent results about plasma parameters characterization in quiescent and turbulent Electron Cyclotron Resonance-heated plasmas will be given. A complete characterization has been already performed, studying, in particular, the time evolution of X-ray spectra and the change of plasma morphology, including the balance between radiation originated in the plasma core and the one due to plasma losses. Finally, the experimental setup is going to be further upgraded in order to allow measurements of nuclear decays in magnetoplasmas.

The ORNL Deuterated Spectroscopic Array — ODeSA

Abstract An array consisting of 12 deuterated organic liquid scintillator detectors for fast-neutron spectroscopy was designed and built at Oak Ridge National Laboratory (ORNL). This versatile array is designed for measurements with low reaction yields, such as those performed with rare isotope beams, as well as at high current DC facilities used for underground nuclear astrophysics research. Because some measurements also offer limited, or no, additional timing information, the ORNL Deuterated Spectroscopic Array (ODeSA) was optimized to utilize spectrum unfolding to extract neutron energy spectra . This array was characterized for n/ γ pulse shape discrimination, light response, resolution, and intrinsic efficiency by using the neutron time-of-flight tunnel at the Edwards Accelerator Laboratory at Ohio University. Results and future plans are discussed.

From Nuclei to the Cosmos: Tracing Heavy-Element Production with the Oldest Stars

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.

The Soreq Applied Research Accelerator Facility (SARAF): Overview, research programs and future plans

The Soreq Applied Research Accelerator Facility (SARAF) is under construction in the Soreq Nuclear Research Center at Yavne, Israel. When completed at the beginning of the next decade, SARAF will be a user facility for basic and applied nuclear physics, based on a 40 MeV, 5 mA CW proton/deuteron superconducting linear accelerator. Phase I of SARAF (SARAF-I, 4 MeV, 2 mA CW protons, 5 MeV 1 mA CW deuterons) is already in operation, generating scientific results in several fields of interest. The main ongoing program at SARAF-I is the production of 30 keV neutrons and measurement of Maxwellian Averaged Cross Sections (MACS), important for the astrophysical s-process. The world leading Maxwellian epithermal neutron yield at SARAF-I ($5\times 10^{10}$ epithermal neutrons/sec), generated by a novel Liquid-Lithium Target (LiLiT), enables improved precision of known MACSs, and new measurements of low-abundance and radioactive isotopes. Research plans for SARAF-II span several disciplines: Precision studies of beyond-Standard-Model effects by trapping light exotic radioisotopes, such as $^6$He, $^8$Li and $^{18,19,23}$Ne, in unprecedented amounts (including meaningful studies already at SARAF-I); extended nuclear astrophysics research with higher energy neutrons, including generation and studies of exotic neutron-rich isotopes relevant to the rapid (r-) process; nuclear structure of exotic isotopes; high energy neutron cross sections for basic nuclear physics and material science research, including neutron induced radiation damage; neutron based imaging and therapy; and novel radiopharmaceuticals development and production. In this paper we present a technical overview of SARAF-I and II, including a description of the accelerator and its irradiation targets; a survey of existing research programs at SARAF-I; and the research potential at the completed facility (SARAF-II).

How were the heavy chemical elements beyond iron made in the Universe?

Nuclear astrophysics, which is an interdisciplinary branch of nuclear physics (micro scale) and astrophysics (macro scale), addresses some of the most compelling questions in the universe. Research efforts have been devoted to many topics such as the origins of the chemical elements, the unique conditions of earth that makes life possible, and the formation and evolution of the sun, stars, and galaxies. Nuclear processes play an extremely important role in cosmic evolution after the Big Bang, and they are the only known mechanisms that synthesize heavy elements, in addition to providing the energy for stars to resist the force of gravity. Over the past 50 years, scientists have developed a deep understanding of Big-Bang primordial nucleosynthesis and the mechanisms for synthesizing heavy elements. However, the astrophysical models have yet to adequately reproduce the observed solar abundances of those elements beyond iron (referred to as ultra-iron elements). It is widely believed that these ultra-iron elements were primarily synthesized via the slow neutron capture process (s-process) and the fast neutron capture process (r-process). The fundamental s-process component is thought to originate from thermally pulsing low-mass AGB stars, with reaction pathways closed after the stable nuclides. About half of the heavy elements (up to bismuth) were produced via the s-process. The r-process is thought to occur in the explosive burning of core-collapse supernova and/or neutron-star mergers. Although the r-process site remains a mystery, experts believe that more than half of the ultra-iron elements (up to thorium and uranium) were produced via the r-process. In addition, there are 35 neutron-deficient stable isotopes, which are present in significantly less abundance in our solar system. These so-called p-nuclei are likely produced in Type II supernova, through the photo-dissociation (referred to as p-process or r-process) of existing s- or r-process seeds, or through the recently proposed neutrino-proton v p-process. Astrophysical models require a huge amount of nuclear-physics input data. The most essential data include nuclear mass, structure, decay and fission characteristics, and related nuclide cross-sections along the various nucleosynthesis paths. Thus far, the lack of systematic and precise nuclear inputs is one of the main reasons scientists have not been able to reproduce the observed solar abundances of ultra-iron elements. Published by Discover magazine in 2002, the American National Research Council ranked the question, how were the heavy elements from iron to uranium made? as one of the 11 Greatest Unanswered Questions of Physics in this Century . More complete and precise nuclear physics inputs are therefore urgently needed to improve astrophysical models and decode the observations. This paper introduces the most important nucleosynthesis processes that are responsible for the ultra-iron elements production in the universe, while also summarizing the relevant key nuclear-physics inputs required in the astrophysical models. Finally, the frontier in this field study includes the origins of ultra-iron elements, and the future of nuclear astrophysics research in China is examined.

Production of negatively charged radioactive ion beams**This manuscript has been authored by UT-Battelle, LLC under Contract No. DE-AC05-00OR22725 with the US Department of Energy. The United States Government retains and the publisher, by accepting the article for publication, acknowledges that the United States Government retains a non-exclusive, paid-up, irrevocable, world-wide license to publish or reproduce the published form of this

Beams of short-lived radioactive nuclei are needed for frontier experimental research in nuclear structure, reactions, and astrophysics. Negatively charged radioactive ion beams have unique advantages and allow for the use of a tandem accelerator for post-acceleration, which can provide the highest beam quality and continuously variable energies. Negative ion beams can be obtained with high intensity and some unique beam purification techniques based on differences in electronegativity and chemical reactivity can be used to provide beams with high purity. This article describes the production of negative radioactive ion beams at the former holifield radioactive ion beam facility at Oak Ridge National Laboratory and at the CERN ISOLDE facility with emphasis on the development of the negative ion sources employed at these two facilities.

Preparation of 7Be targets for nuclear astrophysics research

This work describes the preparation of three 7Be targets which were used in two independent measurements of the 7Be(n,α)4He cross section in the energy range of interest for the Big-Bang nucleosynthesis at the n_TOF-CERN facility and at Soreq-SARAF . A more precise value of this cross section could shed light on the long lasting "Cosmological Lithium problem". Two methods for target preparation were used. A target was obtained by deposition and subsequent air-drying of (24.50± 0.54) GBq of Be(NO3)2 droplets precisely positioned onto a stretched low density polyethylene film 0.635 μm thick. The thickness of the deposited Be(NO3)2 layer was deduced using Monte-Carlo simulations to be 0.36 μm. The energy loss of 8500 keV alpha particles passing through the target obtained by air-drying of 7Be(NO3)2 droplets was estimated to be 88 keV . Two other targets were prepared via molecular plating onto ∼ 5 μm and 1 mm thick aluminium backings, respectively. The first was obtained by molecular plating (24.47± 0.53) GBq of 7Be, resulting in a deposited layer of Be(OH)2, 1.04 μm thick. The second molecular plated target was obtained depositing (3.95± 0.08) GBq of 7Be. The mean energy loss of 8500 keV alpha particles, passing through the molecular plated target with 5 μm thick aluminium backings was estimated as 814 keV . The energy loss by 8500 keV alpha particles in all the obtained targets is considered tolerable for the envisaged cross section measurements. The preparation and characterization of the targets is here described.

And so it all began: A personal tribute to the man behind the scientist

At the time I began my scientific career as a PhD student under the supervision of Claudio Spitaleri, the Trojan Horse Method was still in its infancy. Like with any new-born idea, it took time and passion and effort to plant the early seeds that would eventually develop into a now well-established method in nuclear astrophysics research. Here, I offer my own recollection of those early years as a personal homage to Claudio’s unique mix of human traits that shaped our professional relationship for many years since.