A5024200119- Nuclear physics research studies
- Nuclear Physics and Applications
- Astronomical and nuclear sciences
- Atomic and Subatomic Physics Research
- Gamma-ray bursts and supernovae
- Nuclear reactor physics and engineering
- Radiation Detection and Scintillator Technologies
- Astro and Planetary Science
- Particle physics theoretical and experimental studies
- Spectroscopy and Laser Applications
- Quantum, superfluid, helium dynamics
- Atmospheric Ozone and Climate
- Neutrino Physics Research
- Radiation Therapy and Dosimetry
- Advanced NMR Techniques and Applications
- Stellar, planetary, and galactic studies
- Particle Detector Development and Performance
- Algorithms and Data Compression
University of Naples Federico II
2022-2025
Istituto Nazionale di Fisica Nucleare, Sezione di Napoli
2021-2025
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...
In nuclear astrophysics, the accurate determination of reaction cross sections at astrophysical energies is critical for understanding stellar evolution and nucleosynthesis. This study focuses on $^{12}$C($p, \gamma$)$^{13}$N reaction, which takes part in CNO cycle significant determining $^{12}$C/$^{13}$C ratio interiors. Data from various studies, including recent LUNA measurements, reveal high discrepancies section values, underscoring need robust fitting approaches. Utilizing R-matrix...
In nuclear astrophysics, the accurate determination of reaction cross sections at astrophysical energies is critical for understanding stellar evolution and nucleosynthesis. This study focuses on $^{12}\mathrm{C}(p,\ensuremath{\gamma})^{13}\mathrm{N}$ reaction, which takes part in CNO cycle significant determining $^{12}\mathrm{C}/^{13}\mathrm{C}$ ratio interiors. Data from various studies, including recent LUNA measurements, reveal high discrepancies cross-section values, underscoring need...
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...
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.
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...
In deep-underground experiments, intrinsic detector background can exceed the external one, limiting detection sensitivity. Intrinsic in liquid scintillator neutron detectors consists of alpha particles emitted from radioactive impurities housing (and possibly liquid). We present results long measurements 12 EJ-309 organic scintillators Gran Sasso National Laboratory Italian Institute Nuclear Physics. These are a part array for SHADES ERC project that aims to measure very low cross section...
Neutron capture reactions are the main contributors to synthesis of heavy elements through s-process. Together with 13 C( α , n) 16 O, which has recently been measured by LUNA collaboration in an energy region inside Gamow peak, 22 Ne( 25 Mg is other neutron source stars. Its cross section mostly unknown relevant stellar (450 keV < E cm 750 keV), where only upper limits from direct experiments and highly uncertain estimates indirect sources exist. The ERC project SHADES (UniNa/INFN) aims...
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...
Nuclear reactions are responsible for the chemical evolution of stars, galaxies and Universe. Unfortunately, at temperatures interest nuclear astrophysics, cross-sections thermonuclear in pico- femto-barn range thus measuring them laboratory is extremely challenging. In this framework, major steps forward were made with advent underground pioneered by Laboratory Underground Astrophysics (LUNA). The cosmic background reduction several orders magnitude obtained LUNA, however, needs to be...
Abstract The 13 C( α , n ) 16 O reaction is the main neutron source of s -process taking place in thermally pulsing AGB stars and it one candidate sources neutrons for i astrophysical sites proposed so far. Therefore, its rate crucial to understand production nuclei heavier than iron Universe. For first time, LUNA collaboration was able measure cross section at E c.m. = 0.23−0.3 MeV drastically reducing uncertainty S ( )-factor astrophysically relevant energy range. In this paper, we provide...
The $\mathrm{^{20}Ne(p, \gamma)^{21}Na}$ 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 $E\rm_{cm} = 352$~keV, contribution from $E^{\rm }_{cm} 368$~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...
The detection of neutrons in low energy astrophysics poses two main problems: cross section measurement requires high efficiency and ideally, beam-induced external neutron backgrounds should be identified through an sensitive detector. In recent years, capture-gated spectroscopy has found new opportunities to grow materials better availability modern data acquisition systems. this work we will present the design, expected capabilities preliminary characterization hybrid detector array...
The ^{12}C/^{13}C ratio is a significant indicator of nucleosynthesis and mixing processes during hydrogen burning in stars. Its value mainly depends on the relative rates ^{12}C(p,γ)^{13}N ^{13}C(p,γ)^{14}N reactions. Both reactions have been studied at Laboratory for Underground Nuclear Astrophysics (LUNA) Italy down to lowest energies date (E_{c.m.}=60 keV) reaching first time high energy tail shell giant Our cross sections, obtained with both prompt γ-ray detection activation...