A. Caciolli
A5060893018- Nuclear physics research studies
- Nuclear Physics and Applications
- Astronomical and nuclear sciences
- Atomic and Molecular Physics
- X-ray Spectroscopy and Fluorescence Analysis
- Neutrino Physics Research
- Astro and Planetary Science
- Quantum Chromodynamics and Particle Interactions
- Particle physics theoretical and experimental studies
- Gamma-ray bursts and supernovae
- Radioactivity and Radon Measurements
- Nuclear reactor physics and engineering
- Radiation Detection and Scintillator Technologies
- Stellar, planetary, and galactic studies
- Atomic and Subatomic Physics Research
- Advanced Chemical Physics Studies
- Inorganic Fluorides and Related Compounds
- Particle accelerators and beam dynamics
- Radiation Therapy and Dosimetry
- Geochemistry and Geologic Mapping
- Radiopharmaceutical Chemistry and Applications
- Atmospheric Ozone and Climate
- X-ray Diffraction in Crystallography
- Catalytic Processes in Materials Science
- Nuclear Materials and Properties
Istituto Nazionale di Fisica Nucleare, Sezione di Padova
2016-2025
University of Padua
2016-2025
Osservatorio Astronomico di Padova
2016
Istituto Nazionale di Fisica Nucleare, Laboratori Nazionali di Legnaro
2012-2015
Sapienza University of Rome
2015
Istituto Nazionale di Fisica Nucleare
2007-2014
Institute for Physics
2014
University of Siena
2011
University of Florence
2006-2007
Recent observations of (6)Li in metal poor stars suggest a large production this isotope during big bang nucleosynthesis (BBN). In standard BBN calculations, the (2)H(α,γ)(6)Li reaction dominates production. This has never been measured inside energy region because its cross section drops exponentially at low and electric dipole transition is strongly suppressed for isoscalar particles (2)H α energies below Coulomb barrier. Indirect measurements using dissociation only give upper limits...
The ^{17}O(p,α)^{14}N reaction plays a key role in various astrophysical scenarios, from asymptotic giant branch stars to classical novae. It affects the synthesis of rare isotopes such as ^{17}O and ^{18}F, which can provide constraints on models. A new direct determination E_{R}=64.5 keV resonance strength performed at Laboratory for Underground Nuclear Astrophysics (LUNA) accelerator has led most accurate value date ωγ=10.0±1.4_{stat}±0.7_{syst} neV, thanks significant background...
The Ne22(p,γ)Na23 reaction takes part in the neon-sodium cycle of hydrogen burning. This affects synthesis elements between Ne20 and Al27 asymptotic giant branch stars novae. rate is very uncertain because a large number unobserved resonances lying Gamow window. At proton energies below 400 keV, only upper limits exist literature for resonance strengths. Previous evaluations differ by factors. In present work, first direct observations at 156.2, 189.5, 259.7 keV are reported. Their strengths...
Abstract Studying interactions of radioactive ions with neutrons is particularly demanding and has been performed only in a few cases. Some these are crucial several astrophysical contexts. In the present work, case 7 Be destruction induced by (n, α ) reaction investigated at energies typical primordial nucleosynthesis means Trojan Horse Method applied to 2 H( Be, αα )p quasi-free reaction. The Be(n, 4 He cross-section measured single experiment from ∼2 MeV down cosmological energies....
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 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...
The rate of the hydrogen-burning carbon-nitrogen-oxygen (CNO) cycle is controlled by slowest process, 14N(p,γ)15O, which proceeds capture to ground and several excited states in O15. Previous extrapolations for state contribution disagreed a factor 2, corresponding 15% uncertainty total astrophysical S factor. At Laboratory Underground Nuclear Astrophysics (LUNA) 400 kV accelerator placed deep underground Gran Sasso facility Italy, new experiment on has been carried out at 317.8, 334.4,...
Background: The O17(p,γ)F18 reaction affects the production of key isotopes (e.g., F18 and O18) in explosive hydrogen burning that powers classical novae. Under these conditions, rate is dominated by contributions from a narrow resonance at Ec.m.=183keV combined direct capture low-energy tails broad resonances. At present, astrophysical not well constrained because lack data energy region appropriate to Purpose: This study aims measurement cross section order determine its temperature...
Proton captures on Mg isotopes play an important role in the Mg–Al cycle active stellar H-burning regions. In particular, low-energy nuclear resonances 25Mg(p, γ)26Al reaction affect production of radioactive 26Algs as well resulting Mg/Al abundance ratio. Reliable estimations these quantities require precise measurements strengths resonances. Based a new experimental study performed at Laboratory for Underground Nuclear Astrophysics, we provide revised rates γ)26Algs and γ)26Alm reactions...
We investigate the impact of new LUNA rate for nuclear reaction $^{22}$Ne$(p,γ)^{23}$Na on chemical ejecta intermediate-mass stars, with particular focus thermally-pulsing asymptotic giant branch (TP-AGB) stars that experience hot-bottom burning. To this aim we use PARSEC and COLIBRI codes to compute complete evolution, from pre-main sequence up termination TP-AGB phase, a set stellar models initial masses in range $3.0\,M_{\odot} - 6.0\,M_{\odot}$, metallicities $Z_{\rm i}=0.0005$,...
The authors perform a direct measurement of radiative proton capture on ${}^{22}$Ne at the LUNA underground laboratory whose low background allows unprecedented sensitivity. They report detailed experimental information for three recently observed new resonances in ${}^{22}$Ne($p$,$\ensuremath{\gamma}$)${}^{23}$Na reaction which is most uncertain process neon-sodium cycle stellar hydrogen burning. At temperatures relevant nucleosynthesis asymptotic giant branch stars and classical novae, its...
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...
Classical novae are important contributors to the abundances of key isotopes, such as radioactive (18)F, whose observation by satellite missions could provide constraints on nucleosynthesis models in novae. The (17)O(p,γ)(18)F reaction plays a critical role synthesis both oxygen and fluorine but its rate is not well determined because lack experimental data at energies relevant explosions. In this study, cross section has been measured directly for first time wide energy range E(c.m.)~/=...