Nuclear Astrophysics Research Papers - Academia.edu (original) (raw)

2025, Bulletin of the American Physical Society

The origin of the elements from roughly zinc-to-tin (30<Z<50) has yet to be determined. The neutron-rich neutrino driven wind of core collapse supernova (CCSN) is a proposed site for the nucleosynthesis of these elements. However, a significant source of uncertainty exists in elemental abundance yields from astrophysics model calculations due to the uncertainty for (α, n) reaction rates, as most of the relevant cross sections have yet to be measured. We are developing a neutron long counter tailored to measure neutrons for (α, n) reaction measurements performed at The Ohio University Edwards Accelerator Laboratory. The detector design will be optimized using the Monte-Carlo N-Particle transport code (MCNP6). Details of the optimization process, as well as the present status of the detector design will be provided. The plans for first (α, n) cross section measurements will also be briefly discussed.

2025, Bulletin of the American Physical Society

Submitted for the DNP12 Meeting of The American Physical Society 18 Ne level structure and the 14 O(α,p) reaction rate WAN-PENG TAN, S. ALMARAZ-CALDERON, A. APRAHAMIAN, B. BUCHER, A. ROBERTS, M. WIESCHER, University of Notre Dame, C. BRUNE, T. MASSEY, Ohio University, N. OZKAN, R. GURAY, Kocaeli University, H. MACH, Uppsala University -On one of the hot CNO waiting points, the 14 O(α,p) reaction plays an important role in explosive hydrogen burning environments like X-ray bursts. It proceeds through the resonances (above the alpha-decay threshold) in 18 Ne. The level structure of 18 Ne above the alpha-decay threshold has been studied using the 16O ( 3 He,n) reaction at Notre Dame. A coincidence measurement of neutrons and charged particles decaying from populated states in 18 Ne has been made. Decay branching ratios were measured for six resonances and used to calculate the 14 O(α,p) 17 F reaction rate. The new experimental information combined with previous experimental and theoretical information provides a more accurate calculation of the reaction rate.

2025, Proceedings of the 12th Asia Pacific Physics Conference (APPC12)

2025

This paper presents a conceptual framework that reinterprets black hole collapse as the source of emergent cosmological spacetime. In full accordance with Schwarzschild geometry, the model replaces the classical collapse into a singularity with dynamically structured, null-ordered layers of redshifted matter accumulating on the horizon, as seen by an external observer. The black hole initially forms on the Planck scale and acts as a source of gravity, with the event horizon dynamically growing outward. This growth generates a causal sequence of redshifted layers on the horizon, with radial motion asymptotically frozen due to gravitational time dilation, while angular and lateral modes remain unconstrained and dynamically active. The resulting surface structure holographically encodes information that projects an internally expanding universe. Topologically, however, the interior of the black hole is absent, the event horizon represents the ultimate boundary of the causal structure. This framework provides a physical realization of the holographic principle and a causal mechanism for the emergence of cosmic time, entropy gradients, and structure formation, while preserving unitarity and respecting entropy bounds. The model offers a complementary, geometrically motivated interpretation of horizon dynamics that bridges black hole thermodynamics, holography, and cosmology, uniting general relativity, quantum theory, and the origin of cosmic structure.

2025, Physical review letters

We report on the measurement of the ^{7}Be(n,p)^{7}Li cross section from thermal to approximately 325 keV neutron energy, performed in the high-flux experimental area (EAR2) of the n_TOF facility at CERN. This reaction plays a key role in the lithium yield of the big bang nucleosynthesis (BBN) for standard cosmology. The only two previous time-of-flight measurements performed on this reaction did not cover the energy window of interest for BBN, and they showed a large discrepancy between each other. The measurement was performed with a Si telescope and a high-purity sample produced by implantation of a ^{7}Be ion beam at the ISOLDE facility at CERN. While a significantly higher cross section is found at low energy, relative to current evaluations, in the region of BBN interest, the present results are consistent with the values inferred from the time-reversal ^{7}Li(p,n)^{7}Be reaction, thus yielding only a relatively minor improvement on the so-called cosmological lithium problem. ...

2025, Physical Review C

The liquid-gas phase transition in hot asymmetric nuclear matter is investigated within relativistic mean-field model using the density dependence of nuclear symmetry energy constrained from the measured neutron skin thickness of finite nuclei. We find symmetry energy has a significant influence on several features of liquid-gas phase transition. The boundary and area of the liquid-gas coexistence region, the maximal isospin asymmetry and the critical values of pressure and isospin asymmetry all of which systematically increase with increasing softness in the density dependence of symmetry energy. The critical temperature below which the liquid-gas mixed phase exists is found higher for a softer symmetry energy.

2025, Physical Review A

The electron-positron pairs observed in heavy-ion collisions at Gesellschaft für Schwerionenforschung Darmstadt mbH have been interpreted as the decay products of yet unknown particles with masses around 1.8 MeV. The negative results of resonant Bhabha scattering experiments, however, do not Support such an interpretation. Therefore we focus on a more complex decay scenario, where the e +e -lines result from a two-collision process. We discuss the induced decay of a metastable 1 + + state into e + e -pairs. For most realizations of a 1 + + state such a decay in leading order can only take place in the Coulomb field of a target atom. This fact has the attractive consequence that for such a state the Bhabha bounds are no longer valid. However, the absolute value of the e ' e production Cross section tums out to be unacceptably small.

2025, Proceedings of International Symposium on Nuclear Astrophysics - Nuclei in the Cosmos - IX — PoS(NIC-IX)

The neutron capture cross sections of 90,91,92,94,96 Zr, which play a key role for the determination of the neutron density in the He burning zone of the Red Giant stars, were measured over the energy range from 1 eV to 1 MeV at the spallation neutron facility n_TOF at CERN. Based on these data the capture resonance strength and the Maxwellian-averaged cross section at 30 keV were calculated.

2025

The neutron time of flight (n_TOF) facility at CERN is a spallation neutron source with white neutron energy spectrum (from thermal to several GeV), covering the full energy range of interest for nuclear astrophysics, in particular for measurements of the neutron capture cross section required in s-process nucleosynthesis. This contribution presents an overview on the astrophysical program carried on at the n_TOF facility, the main results and their implications.

2025, AIP Conference Proceedings

A series of measurements of 237 Np fission cross section have been performed at the CERN spallation neutron facility n_TOF which covers a wide energy range from 1 eV up to 250 MeV. A fast ionization chamber (FIC) was used as a fission fragment detector with registration efficiency of not less than 97 %. Particular attention was paid to correct the fission

2025, AIP Conference Proceedings

All the stable lead isotopes and 209 Bi have been recently measured at n_TOF [1] (CERN) in the range from 1 eV up to 1 MeV, using an optimized experimental setup. A set of two homemade C 6 D 6 detectors with carbon-fibre canning was designed to greatly reduce the sensitivity to scattered neutrons. Surrounding elements like the sample holder and the sample exchanger have been made also of carbon fibre. The pulse-height weighting technique has been used in order to determine the (n,γ) cross sections. Concerning this technique, special care has been taken in the treatment of several sources of error leading to a total systematic uncertainty of less than 3%. Results on the analysed 209 Bi and 207 Pb capture data and a comparison with previous experiments and evaluations are presented.

2025, AIP Conference Proceedings

2025, Physical Review C

Because the relatively small neutron capture cross sections of the zirconium isotopes are difficult to measure, the results of previous measurements are often not adequate for a number of problems in astrophysics and nuclear... more

2025, Physical Review C

The 151 Sm(n, γ ) cross section was measured with the time-of-flight technique from 0.6 eV up to 1 MeV relative to the Au standard with an overall uncertainty of typically 6%. Neutrons were produced by spallation at the innovative n TOF facility at CERN; the γ rays from capture events were detected with organic C 6 D 6 scintillators. Experimental setup and data analysis procedures are described with emphasis on the corrections for detection efficiency, background subtraction, and neutron flux determination. At low energies, resonances could be resolved up to about 1 keV, yielding a resonance integral of 3575 ± 210 b, an average s-wave resonance spacing of D 0 = 1.49 ± 0.07 eV, and a neutron strength function of S 0 = (3.87 ± 0.33) × 10 -4 . Maxwellian-averaged capture cross sections are reported for thermal energies between 5 and 100 keV. These results are of relevance for nuclear structure studies, nuclear astrophysics, and nuclear technology. The new value of the Maxwellian-averaged cross section at kT = 30 keV is 3.08 ± 0.15 b, considerably larger than previous theoretical estimates, and provides better constraints for the thermodynamic conditions during the occurrence of the slow neutron capture process in low-mass stars during their asymptotic giant branch phase.

2025, Journal of Physics: Conference Series

2025

In this paper we describe the main characteristics and the most relevant results obtained at the neutron Time-Of-Flight (n TOF) facility. This experiment is running at CERN in Geneva and concern the measurements of the neutron capture and neutron fission cross sections. In particular we illustrate the mechanisms of neutron production, the characteristics of the neutron beam, the main experimental apparata and the data analysis procedures. Finally we review the most important results with particular care to the implications in the Nuclear Astrophysics and the experimental program planned for the next years.

2025, The European Physical Journal A

In extreme astrophysical environments such as core-collapse supernovae and binary neutron star mergers, neutrinos play a major role in driving various dynamical and microphysical phenomena, such as baryonic matter outflows, the synthesis of heavy elements, and the supernova explosion mechanism itself. The interactions of neutrinos with matter in these environments are flavorspecific, which makes it of paramount importance to understand the flavor evolution of neutrinos. Flavor evolution in these environments can be a highly nontrivial problem thanks to a multitude of collective effects in flavor space, arising due to neutrino-neutrino (ν-ν) interactions in regions with high neutrino densities. A neutrino ensemble undergoing flavor oscillations under the influence of significant ν-ν interactions is somewhat analogous to a system of coupled spins with long-range interactions among themselves and with an external field ('long-range' in momentum-space in the case of neutrinos). As a result, it becomes pertinent to consider whether these interactions can give rise to significant quantum correlations among the interacting neutrinos, and whether these correlations have any consequences for the flavor evolution of the ensemble. In particular, one may seek to utilize concepts and tools from quantum information science and quantum computing to deepen our understanding of these phenomena. In this article, we attempt to summarize recent work in this field. Furthermore, we also present some new results in a three-flavor setting, considering complex initial states.

2025, Nuclear Physics A

High spin states at 12.0-17.6 MeV in 'sSi excited through the '%("Ne, CX) reaction have been investigated with a particle-particle angular correlation method. New spin-parity assignments ranging from 3-to lO+ have been made, some of which are classified into an excited prolate band reported previously. Most states in this energy region are found to decay both by alpha and proton emission. Specifically, a new 6+ state found at 12.80 MeV is identified to be the lowest excited state whch has a large fraction of g9,2 component. This is also supported by a successful reanalysis of the "Al( (x, t)**Si reaction at 65 MeV by a DWBA calculation assuming g,,, transfer. These high-lying states also are discussed in terms of coexistence of oblate and prolate shape bands in %i. The particle decay property of these states in **Si is also discussed comparatively with that in %. NUCLEAR REACTION '*C("Ne, a), E = 52 MeV; measured excitation energies, ~(0). E aa (0), ap( 0). %i deduced branching ratios of p. Q decays, J, ?r, particle decay characteristics, coexistence of oblate, prolate bands and excited prolate band.

2025, Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment

A low-background gamma-ray detector of NaI(Tl) comprising a core surrounded by an annulus was developed for nuclear astrophysics experiments with radioactive ion beams, mostly for detailed studies of low-energy radiative capture reactions that involve proton and alpha particles. Monte Carlo simulations using EGS4 were performed to calculate the full-energy detection e$ciency. The background was satisfactorily reduced as designed. The best S/N ratio for very low-event rate was obtained using the annulus in anticoincidence with the core. A consideration of an experiment of astrophysical interest, the Ne(p, )Na reaction, is also brie#y discussed.

2025, Zeitschrift f�r Physik A: Hadrons and Nuclei

Atomic nuclear clusters play a crucial role in nucleosynthesis in the universe, especially in the main sequence of heavy element synthesis. Cluster aspects in nucleosynthesis are briefly discussed based on a Cluster-Nucleosynthesis Diagram proposed here. Two recent topics on critical a-induced thermonuclear reactions are reviewed; the first one is the 12C(~, ~)160 reaction for the He burning stage and the other one is the 8Li(e, n)llB reaction for the big bang nucleosynthesis. A new field of nuclear astrophysics using radioactive nuclear beams is also discussed. As the stars evolve, the nucleosynthesis processes go faster, and finally they come to the point of a gravitational collapse if the mass of the star is large, which leads to a supernova explosion. Or, it may stop by becoming a white dwarf if the mass is small. Each step of the stellar evolution is characterized by a specific nucleosynthesis. Thus, one can test critically the standard model of the stellar evolution by studying the nuclear reaction processes which are not well known yet. These works eventually give enough nuclear physics information to deduce the information on the stellar environment of interest. These are the main subjects of nuclear astrophysics. Of course, the nucleosynthesis scenarios have been checked by the astronomical observations, meteorite studies, cosmic rays, etc.

2025, The European Physical Journal A

An in-flight RIB separator at low energies, which is the first extensive separator at low energies, called CRIB, is just under construction at CNS. This consists of a double-achromatic magnetic separator, a window-less gas target, and a Wien filter. Some characteristics of the CRIB are described. Possible experimental plans are also discussed in our nuclear astrophysics project for the study of the explosive hydrogen burning process, especially on the onset mechanism.

2025

Determination of Neutron Branching in 12 C+ 12 C Fusion 1 JUSTIN BROWNE, University of Notre Dame -The neutron branch of the 12 C+ 12 C is important for the carbon shell burning and carbon explosive burning. The 23 Mg created by the 12 C( 12 C,n) 23 Mg reaction may undergo β + decay, changing the neutron excess in the combusting material, and the neutrons emitted from this reaction may contribute to s-and r-processes. Both the β + decay and the neutron emission greatly affect the subsequent nucleosynthesis in the star. A detection system, consisting of an array of four plastic scintillators and two Germanium detectors, has been developed to detect the decay of the 23 Mg. The system has been tested at E c.m. = 4.24MeV. Using β + -γ coincidence technique, the 23 Mg reaction products has been unambiguously identified.

2025

The Active Target Time Projection Chamber (AT-TPC) at Michigan State University (MSU) will be filled with a gas that is used as both the target and the detector. To determine the intensity of the beam as it enters the chamber, a detector must be placed immediately upstream of the AT-TPC. The beam intensity is measured by passing the beam through a foil and measuring the amount of ionization in the foil. Because the signal from the primary electrons would be too weak, the electrons are multiplied in a Multichannel Plate (MCP) detector. The electrons are transported out of the beam path to the MCP by electric and magnetic fields.

2025

Minimizing Residual Pressure within a Windowless Gas Target System -JENSA ORLANDO GOMEZ, Floirda International University, JUSTIN BROWNE, ANTONIOS KONTOS, FERNANDO MONTES, Michigan State University, JENSA COLLABORATION -Nuclear reactions between light gases and radioactive isotope beams are essential to address open questions in nuclear structure and astrophysics. Pure light gas targets are critical for the measurements of proton-and alpha-induced reactions. Jet Experiments in Nuclear Structure and Astrophysics (JENSA) is the world's most dense (∼ 10 19 atoms/cm 2 ) windowless gas target system. Most of the gas flow is localized; however, escaping gas creates a pressure gradient which degrades experimental measurements and contaminates the beam line. JENSA contains a differential pumping system to maintain a vacuum. The previous design configuration was not optimized for experiments (pressure measurements 70 cm downstream from the jet were ∼ 10 -3 torr; optimal is less than 10 -4 torr). We have altered the current differential pumping system to minimize the residual pressure profile. Several configurations of two gas-receiving catchers were tested, and the most efficient ones identified using Enhanced Pirani and Cold Cathode gauges. We have determined the 30 mm outer and 20 mm inner gas-receiving cones minimize JENSA central chamber pressure to 200 millitorr at 16,000 torr of discharge pressure. Altering the tubing configuration has additionally lowered the pressure 70 cm downstream to 10 -5 torr. The new residual pressure allows operation of JENSA with planned expansion of a recoil mass separator SECAR.

2025, Nuclear Physics

The existence of a cosmic neutrino background -the analogue of the cosmic microwave background -is a fundamental prediction of standard big bang cosmology. Up to now, the observational evidence for its existence is rather indirect and rests entirely on cosmological observations of, e.g., the light elemental abundances, the anisotropies in the cosmic microwave background, and the large scale distribution of matter. Here, we review more direct, weak interaction based detection techniques for the cosmic neutrino background in the present epoch and in our local neighbourhood. We show that, with current technology, all proposals are still off by some orders of magnitude in sensitivity to lead to a guaranteed detection of the relic neutrinos. The most promising laboratory search, based on neutrino capture on beta decaying nuclei, may be done in future experiments designed to measure the neutrino mass through decay kinematics.

2025, Nuclear Physics B - Proceedings Supplements

We describe and discuss recently proposed improvements of nuclear physics input for the solar neutrino problem, a new parameterization of the resonance cross-section in the complexenergy plane, and a new fusion rate formula.

2025, Research gate

We present a paradigm-shifting mechanism for stellar explosions within the Tanfarid Quantum Thermodynamic Universe (TQTU) framework. Contrary to gravitational-collapse models, we propose coherent electromagnetic self-annihilation as the central driver of supernovae. This process is triggered by destructive interference between a star's native magnetic field (Bn) and a QVP-amplified "waste field" (Bw) from nuclear byproducts, leading to: • Magnetic pressure collapse • Runaway plasma instabilities • Topological reconnection failure • QVP-mediated quantum ignition Key Innovations: 1. First mathematical framework for magnetic self-annihilation in stars 2. Solves 5 outstanding problems in supernova theory 3. Predicts testable EM precursors for next-gen observatories

2025, Journal of Physics: Conference Series

Next generation of radioactive ion beam facilities like FAIR will open a bright future for nuclear structure and nuclear astrophysics research. In particular, very exotic nuclei (mainly neutron rich) isotopes will be produced and a lot of new exciting experimental data will help to test and improve the current nuclear models. In addition, these data (masses, reaction cross sections, beta decay half-lives, etc.) combined with the development of better theoretical approaches will be used as the nuclear physics input for astrophysical simulations. In this presentation I will review some of the state-of-the-art nuclear structure methods and their applications.

2025, EPJ Web of Conferences

One of the most puzzling problems in Nuclear Astrophysics is the "Cosmological Lithium Problem", i.e the discrepancy between the primordial abundance of 7 Li observed in metal poor halo stars , and the one predicted by Big Bang Nucleosynthesis (BBN). One of the reactions that could have an impact on the problem is 7 Be(n,p) 7 Li. Despite of the importance of this reaction in BBN, the cross-section has never been directly measured at the energies of interest for BBN. Taking advantage of the innovative features of the second experimental area at the n_TOF facility at CERN, an accurate measurement of 7 Be(n,p) cross section has been recently performed at n_TOF, with a pure 7 Be target produced by implantation of a 7 Be beam at ISOLDE. The experimental procedure, the setup used in the measurement and the results obtained so far will be here presented.

2025, Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment

An 60 Fe target for studying the 60 Fe(n, g) 61 Fe cross-section at stellar energies was prepared using radiochemical separation techniques. In total, 7.8 Â 10 15 60 Fe atoms (777 ng) were separated from a copper beam dump for the 590 MeV proton beam of the high intensity accelerator at PSI. The final target was prepared by evaporating the iron-containing aqueous solution onto a graphite backing. With this sample the keV neutron capture cross-section of 60 Fe has been measured at FZ Karlsruhe. The work is part of the ERAWAST-initiative (Exotic Radionuclides from Accelerator WAste for Science and Technology) which is aimed at extracting rare valuable radionuclides from accelerator waste by chemical means.

2025

elds on the approach to the Cauchy horizon singularity. We study the behavior of the Weyl scalars 0 and 4 and of the curvature scalar R R , and confront our results with those of perturbation analysis. Our results may be useful when... more

2025, Universe

An accurate measurement of the 140Ce(n,γ) energy-dependent cross-section was performed at the n_TOF facility at CERN. This cross-section is of great importance because it represents a bottleneck for the s-process nucleosynthesis and determines to a large extent the cerium abundance in stars. The measurement was motivated by the significant difference between the cerium abundance measured in globular clusters and the value predicted by theoretical stellar models. This discrepancy can be ascribed to an overestimation of the 140Ce capture cross-section due to a lack of accurate nuclear data. For this measurement, we used a sample of cerium oxide enriched in 140Ce to 99.4%. The experimental apparatus consisted of four deuterated benzene liquid scintillator detectors, which allowed us to overcome the difficulties present in the previous measurements, thanks to their very low neutron sensitivity. The accurate analysis of the p-wave resonances and the calculation of their average parameter...

2025, Physical Review C

Resonance energies E λ , neutron widths n,λ , and radiation widths γ ,λ for the compound system 175 Lu + n were determined up to 1 keV from time-of-flight data reported in literature and recently measured at the GELINA facility of JRC-Geel (Belgium). The statistical analysis of the obtained resonance parameters provides an swave neutron strength function [S 0 = 1.96( )], mean level spacing [D 0 = 3.24(9) eV], and average radiation width ( γ 0 = 61.3(59) meV) which are substantially different from those compiled in libraries dedicated to statistical calculations. The largest difference lies on the average radiation width, for which a value of 77(5) meV is recommended. 175 Lu neutron cross sections were calculated with the TALYS code by using our s-wave average parameters as constraints. At kT = 30 keV, we obtain a total neutron capture cross section equal to 1125(62) mbarns, confirming the lower values reported in the 1990s.

2025, Physical Review C

Cross sections for neutron-induced reactions of 241 Am in the resonance region have been evaluated. Results of time-of-flight cross section experiments carried out at the GELINA, LANSCE, ORELA and Saclay facilities have been combined with optical model calculations to derive consistent cross sections from the thermal energy region up to the continuum region. Resolved resonance parameters were derived from a resonance shape analysis of transmissions, capture yields, and fission yields in the energy region up to 150 eV using the REFIT code. From a statistical analysis of these parameters, a neutron strength function (10 4 S 0 = 1.01 ± 0.12), mean level spacing (D 0 = 0.60 ± 0.01 eV) and average radiation width ( γ 0 = 43.3 ± 1.1 meV) for s-wave resonances were obtained. Neutron strength functions for higher partial waves (l > 0) together with channel and effective scattering radii were deduced from calculations based on a complex mean-field optical model potential, applying an equivalent hard-sphere scattering radius approximation.

2025, Global Journal of Science Frontier Research: Physics and Space Science

Unity is defined as matter or a system with its maximum energy limit. Unity Force is matter’s tendency of being unity, expressed as attracting while energy sharing in a unity or repelling while excess-energy releasing out of the unity. The universe was (and still is) formed of four base particles: proton, electron, neutrino, and photon, created from the Big Bang.Then, each electron bonded with a photon as an electron unity, so that light could not propagate; each proton bonded with a neutrino as a proton unity, and the two unities made the universe opaque. No gravity, nor gravitational collapse, is needed to draw these base particles together because they were dense and hot in the first place when created. The high density and temperature were perfect for nuclear fusions, and the force of nuclear fusion (unity force) would keep pulling particles together. Most nuclear fusion centres with excess-energy releasing, form stars and planets. The rest, extra-large nuclear fusion centres with inner cores unable to release excess-energy as a repelling force, form black holes with much stronger attracting unity forcesof their respective galaxies. Nuclear fusion produced the first light, and then atom formation brought the dawn of the universe. The orbit of each planet was decided by its position on the disk edge of the star system and is fundamentally decided by unity force. As the third planet from the sun, Earth is not too far, not too close, in a right position to have water mostly in liquid state, to nurturebiological organisms and raise our human beings.Unity force forms the hierarchical structure of each galaxy, making the black hole as the galaxy’s unity centre. The observations of “accelerating expansion” of the universe needs larger sample size, randomization, repetition and better calculation.

2025, arXiv (Cornell University)

Solving grand challenges in Nuclear Physics (NP) requires the development of fundamentally new tools for simulation and sensing. U.S. Nuclear Science is in an early stage of benefiting from and contributing to the advancement of Quantum Information Science and Technology (QIST). To capitalize on this progress, we recommend: • Increasing support for driving advances at the interface of NP and QIST to uniquely address Nuclear Science objectives. This support will advance the development of quantum sensor technology for NP; enhance the (co-)development, integration, and application of quantum-based simulation and computation hardware and techniques for NP; grow cross-cutting research and partnerships that leverage NP expertise to accelerate advances in QIST (including access to forefront hardware and fabrication); and expand the training of, and robust professional pathways for, a diverse and inclusive quantum-ready workforce for NP, with cross-disciplinary collaborations in QIST. • Establishing an 'NP Quantum Connection' that will realize the transformational potential of QIST in addressing NP grand challenges. This national initiative will enable a community-wide integration of quantum sensing and simulation in NP research; facilitate sharing of resources and expertise among NP, interagency programs, and the national and international QIST community; support bridge junior faculty and scientist positions, postdoctoral fellowships, and graduate and undergraduate students; and strengthen ties with the QIST community, technology companies, and other domain sciences.

2025, Journal of emerging technologies and innovative research

A Neutron star is formed when an ordinary star dies and a rotating Neutron star is called a Pulsar. Study of pulsars have also been beneficial for time keeping as they are considered among the most accurate known natural time keepers. The current work is used to analyse the time period of a Pulsar using the secondary data from NASA data archive. INTRODUCTION: Pulsars are quickly rotating, extremely magnetised neutron stars that were first seen through pulsed radio emission at a very down radio observing frequency of 81 MHz. A pulsar is a highly magnetized rotating neutron star or white dwarf that is emitting a beam of electromagnetic radiation. There are different types of pulsars i.e. CRAB PULSAR and VELA PULSAR. The Crab Nebula is the supernova remnant in the constellation of Taurus. A neutron star that formed when a massive star collapsed. The Vela pulsar is about 1,000 light years away from Earth, spansis about 12 miles in diameter, and makes over 11 complete rotations every sec...

2025, HAL (Le Centre pour la Communication Scientifique Directe)

We have measured the γ-ray line production cross sections in proton-induced nuclear reactions on various target nuclei ( 12 C, 16 O, 24 Mg, 28 Si, 56 Fe) of chemical elements abundant in astrophysical sites (solar flares, the interstellar medium, cosmic compact objects) over the incident energy range of E p = 30 -200 MeV. We carried out experimental campaigns in joint collaboration at the K = 200 separated sector cyclotron of iThemba LABS using a high-energy resolution, high-efficiency detection array composed of 8 Compton-suppressed clover detectors comprising 32 HP-Ge crystals for recording the γ-ray energy spectra. In the current paper, we focus on γ-ray de-excitation lines produced in proton irradiations of nat C and Mylar targets, in particular, on the prominent 4.439 and 6.129 MeV lines of 12 C and 16 O which are among the strongest lines emitted in solar flares and in interactions of low-energy cosmic rays (LECRs) with the gas and dust of the inner galaxy. We report new γ-ray production experimental cross section data for ten nuclear γ-ray lines that we compare to previous low-energy data sets from the literature, to the predictions of the TALYS code of nuclear reactions and to a semi-empirical compilation. In the first approach, performing calculations with default input parameters of TALYS we observed substantial deviations between the predicted cross sections and experimental data. Then, using modified optical model potential (OMP) and nuclear level deformation parameters as input data we generated theoretical excitation functions for the above two main lines fully consistent with experimental data. In contrast, the experimental data sets for the other eight analyzed lines from the two proton-irradiated targets exhibit significant deviations with the predicted cross section values. We also report line-shape experimental data for the line complex observed at E γ = 4.44 MeV in irradiations of the two targets. Finally, we emphasize the astrophysical implications of our results.

2025, The European Physical Journal Plus

The next years will see the completion of several new facilities at Istituto Nazionale di Fisica Nucleare – Laboratori Nazionali del Sud (LNS) opening up new possibilities in the fields of nuclear structure, nuclear dynamics, nuclear astrophysics and applications. These include a new line for high-intensity cyclotron beams, a new facility for in-flight production of radioactive ion beams, the PANDORA plasma trap for multidisciplinary studies and a high-power laser for basic science and applied physics. The nuclear physics community has organized a workshop to discuss the new physics opportunities that will be possible in the middle term (5–7 years) by employing state-of-the-art detection systems. A detailed discussion of the outcome from the workshop is presented in this report.