A5050236927- Nuclear physics research studies
- Nuclear Physics and Applications
- Astronomical and nuclear sciences
- Neutrino Physics Research
- Particle physics theoretical and experimental studies
- Gamma-ray bursts and supernovae
- Atomic and Molecular Physics
- Atomic and Subatomic Physics Research
- Nuclear reactor physics and engineering
- Quantum, superfluid, helium dynamics
- Stellar, planetary, and galactic studies
- Astro and Planetary Science
- Superconducting Materials and Applications
- X-ray Spectroscopy and Fluorescence Analysis
- Radiation Therapy and Dosimetry
- Quantum Chromodynamics and Particle Interactions
- High-Energy Particle Collisions Research
- Advanced NMR Techniques and Applications
- Spectroscopy and Laser Applications
- Radiation Detection and Scintillator Technologies
- Dark Matter and Cosmic Phenomena
- Astrophysics and Cosmic Phenomena
- Atmospheric Ozone and Climate
Helmholtz-Zentrum Dresden-Rossendorf
2023-2025
University of Milan
2019-2024
Istituto Nazionale di Fisica Nucleare, Sezione di Milano
2019-2024
University of Genoa
2021
Istituto Nazionale di Fisica Nucleare, Sezione di Genova
2021
One of the main neutron sources for astrophysical s process is reaction ^{13}C(α,n)^{16}O, taking place in thermally pulsing asymptotic giant branch stars at temperatures around 90 MK. To model nucleosynthesis during this cross section needs to be known 150-230 keV energy window (Gamow peak). At these sub-Coulomb energies, direct measurements are severely affected by low event rate, making us rely on input from indirect methods and extrapolations higher-energy data. This leads an uncertainty...
Abstract Nuclear astrophysics is a field at the intersection of nuclear physics and astrophysics, which seeks to understand engines astronomical objects origin chemical elements. This white paper summarizes progress status field, new open questions that have emerged, tremendous scientific opportunities opened up with major advances in capabilities across an ever growing number disciplines subfields need be integrated. We take holistic view discussing unique challenges regards science,...
Abstract Studies of charged-particle reactions for low-energy nuclear astrophysics require high sensitivity, which can be achieved by means detection setups with efficiency and low backgrounds, to obtain precise measurements in the energy region interest stellar scenarios. High-efficiency total absorption spectroscopy is an established powerful tool studying radiative capture reactions, particularly if combined cosmic background reduction several orders magnitude obtained at Laboratory...
The C12/C13 ratio is a significant indicator of nucleosynthesis and mixing processes during hydrogen burning in stars. Its value mainly depends on the relative rates C12(p,γ)N13 C13(p,γ)N14 reactions. Both reactions have been studied at Laboratory for Underground Nuclear Astrophysics (LUNA) Italy down to lowest energies date (Ec.m.=60 keV) reaching first time high energy tail shell giant Our cross sections, obtained with both prompt γ-ray detection activation measurements, are most precise...
Background: The competing $^{22}\mathrm{Ne}(\ensuremath{\alpha},\ensuremath{\gamma})^{26}\mathrm{Mg}$ and $^{22}\mathrm{Ne}(\ensuremath{\alpha},n)^{25}\mathrm{Mg}$ reactions control the production of neutrons for weak $s$ process in massive asymptotic giant branch (AGB) stars. In both systems, ratio between corresponding reaction rates strongly impacts total neutron budget influences final nucleosynthesis. A number experimental studies have been performed over recent years which necessitate...
The dipole strength of the nuclide 59Co was studied in photon-scattering experiments using bremsstrahlung produced with electron beams energies 8.6 and 12.2 MeV at facility 𝛾ELBE. We identified 130 levels up to an excitation energy 10.5 MeV. quasicontinuum unresolved transitions included analysis spectra intensities branching were estimated on basis simulations statistical 𝛾-ray cascades. photoabsorption cross section neutron-separation determined is compared predictions reaction model as...
In stars, the fusion of $^{22}$Ne and $^4$He may produce either $^{25}$Mg, with emission a neutron, or $^{26}$Mg $\gamma$ ray. At high temperature, ($\alpha,n$) channel dominates, while at low it is energetically hampered. The rate its competitor, $^{22}$Ne($\alpha$,$\gamma$)$^{26}$Mg reaction, and, hence, minimum temperature for dominance, are controlled by many nuclear resonances. strengths these resonances have hitherto been studied only indirectly. present work aims to directly measure...
The $^{12}\mathrm{C}(p,\ensuremath{\gamma})^{13}\mathrm{N}$ reaction is the onset process of both CNO and hot cycles that drive massive star, red asymptotic giant branch novae nucleosynthesis. rate affects final abundances stable $^{12,13}\mathrm{C}$ nuclides with ramifications for meteoritic carbon isotopic $s$-process neutron source strength. Here, an underground measurement cross section reported. present data, obtained at Felsenkeller shallow-underground laboratory in Dresden (Germany),...
Background: Shell hydrogen burning during the asymptotic giant branch (AGB) phase through oxygen isotopes has been indicated as a key process that is needed to understand observed $^{18}\mathrm{O}/^{16}\mathrm{O}$ relative abundance in presolar grains and stellar atmospheres. This ratio strongly influenced by strengths of reactions $^{18}\mathrm{O}(p,\ensuremath{\alpha})^{15}\mathrm{N}$ $^{18}\mathrm{O}(p,\ensuremath{\gamma})^{19}\mathrm{F}$ low-mass AGB stars. While former channel focus...
The Ne20(p,γ)21Na reaction is the slowest in NeNa cycle and directly affects abundances of Ne Na isotopes a variety astrophysical sites. Here we report measurement its direct capture contribution, for first time below Ec.m.=352 keV, contribution from Ec.m.=368 keV resonance, which dominates rate at T=0.03–1.00 GK. experiment was performed deep underground Laboratory Underground Nuclear Astrophysics, using high-intensity proton beam windowless neon gas target. Prompt γ rays were detected with...
The astrophysical Li6(p,γ)Be7 reaction occurs during Big Bang nucleosynthesis and the pre-main sequence main phases of stellar evolution. low-energy trend its cross section remains uncertain, since different measurements have provided conflicting results. A recent experiment reported a resonancelike structure at center-of-mass energy 195 keV, associated to positive-parity state Be7. existence such resonance is still matter debate. We report new measurement performed Laboratory for...
Abstract The Istituto Nazionale di Fisica Nucleare—Laboratori Nazionali del Gran Sasso (LNGS) is one of the largest underground physics laboratory, a very peculiar environment suited for experiments in Astroparticle Physics, Nuclear Physics and Fundamental Symmetries. newly established Bellotti Ion Beam facility represents major advance possibilities studying nuclear processes an environment. A workshop was organized at LNGS framework Mid Term Plan Italy, initiative Division Instituto...
The CNO cycle is one of the most important nuclear energy sources in stars. At temperatures hydrostatic H-burning (20 MK<T<80 MK) ^{17}O(p,γ)^{18}F reaction rate dominated by poorly constrained 64.5 keV resonance. Here, we report on first direct measurements its resonance strength and capture contribution at 142 keV, performed with a new high sensitivity setup LUNA. present ωγ_{(p,γ)}^{bare}=(30±6_{stat}±2_{syst}) peV about factor 2 higher than values literature, leading to...
Nuclear reaction cross sections are essential ingredients to predict the evolution of AGB stars and understand their impact on chemical our Galaxy. Unfortunately, reactions involved often very small challenging measure in laboratories Earth. In this context, major steps forward were made with advent underground nuclear astrophysics, pioneered by Laboratory for Underground Astrophysics (LUNA). The present paper reviews contribution LUNA understanding related nucleosynthesis.
Recent astronomical data have provided the primordial deuterium abundance with percent precision. As a result, big bang nucleosynthesis may provide constraint on universal baryon to photon ratio that is as precise as, but independent from, analyses of cosmic microwave background. However, such requires nuclear reaction rates governing production and destruction are sufficiently well known. Here, new measurement $^{2}\mathrm{H}{(p,\ensuremath{\gamma})}^{3}\mathrm{He}$ cross-section reported....
The stellar evolution and chemical make-up of the Universe are determined by nuclear reactions occurring in a wide variety sites. Precise determinations cross sections these crucial for calculation reaction rates development models. Laboratory Underground Nuclear Astrophysics (LUNA) collaboration has been at forefront direct measurement low energies astrophysical interest last 35 years. many significant results achieved LUNA have made possible due to background conditions uniquely available...