F. Cavanna
A5054866635- Nuclear physics research studies
- Nuclear Physics and Applications
- Astronomical and nuclear sciences
- Neutrino Physics Research
- Particle physics theoretical and experimental studies
- Dark Matter and Cosmic Phenomena
- Atomic and Subatomic Physics Research
- Gamma-ray bursts and supernovae
- Astrophysics and Cosmic Phenomena
- Atomic and Molecular Physics
- Astro and Planetary Science
- Atmospheric Ozone and Climate
- Stellar, planetary, and galactic studies
- Advanced NMR Techniques and Applications
- Nuclear reactor physics and engineering
- Radiation Therapy and Dosimetry
- Radiation Detection and Scintillator Technologies
- Solar and Space Plasma Dynamics
- Particle accelerators and beam dynamics
- Molecular Spectroscopy and Structure
- Italian Literature and Culture
- Advanced Chemical Physics Studies
- Particle Detector Development and Performance
- Educational and Social Studies
- Quantum, superfluid, helium dynamics
Istituto Nazionale di Fisica Nucleare, Sezione di Genova
2014-2025
Istituto Nazionale di Fisica Nucleare, Sezione di Torino
2020-2025
University of Genoa
2012-2020
Forschungszentrum Jülich
2020
RWTH Aachen University
2020
Istituto Nazionale di Fisica Nucleare, Sezione di Milano
2018-2020
University of Milan
2020
Istituto Nazionale di Fisica Nucleare
2019
Universidad Autónoma de Madrid
2019
Istituto Nazionale di Fisica Nucleare, Laboratori Nazionali del Gran Sasso
2019
We present the simultaneous measurement of interaction rates ${R}_{pp}$, ${R}_{\mathrm{Be}}$, ${R}_{pep}$ $pp$, $^{7}\mathrm{Be}$, and $pep$ solar neutrinos performed with a global fit to Borexino data in an extended energy range (0.19--2.93) MeV particular attention details analysis methods. This result was obtained by analyzing 1291.51 days Phase-II data, collected after extensive scintillator purification campaign. Using counts per day $(\mathrm{cpd})/100\text{ }\mathrm{ton}$ as unit, we...
This paper presents a comprehensive geoneutrino measurement using the Borexino detector, located at Laboratori Nazionali del Gran Sasso (LNGS) in Italy. The analysis is result of 3262.74 days data between December 2007 and April 2019. describes improved techniques optimized selection, which includes enlarged fiducial volume sophisticated cosmogenic veto. reported exposure (1.29±0.05)×1032 protons ×year represents an increase by factor two over previous 2015. By observing...
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...
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 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...
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 $Z_{\rm i}=0.0005$,...
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...
We have measured the flux of cosmic muons in Laboratori Nazionali del Gran Sasso at 3800 m w.e. to be (3.432 ± 0.003)⋅ 10−4 m−2s−1 based on ten years Borexino data acquired between May 2007 and 2017. A seasonal modulation with a period (366.3 0.6) d relative amplitude (1.36 ±0.04)% is observed. The phase (181.7 0.4) d, corresponding maximum 1st July. Using inferred from global atmospheric models, we show muon positively correlated temperature measure effective coefficient αT = 0.90 0.02....
Direct measurements of small nuclear reaction cross sections require a low background in the signal region interest to achieve necessary sensitivity. We describe two complementary detector setups that have been used for studies reactions with solid targets at Laboratory Underground Nuclear Astrophysics (LUNA): high-purity germanium and bismuth germanate (BGO) detector. present effect customised lead shielding on measured spectra LUNA. developed model contributions environmental intrinsic...
The $^{22}$Ne($p,\gamma$)$^{23}$Na reaction, part of the neon-sodium cycle hydrogen burning, may explain observed anticorrelation between sodium and oxygen abundances in globular cluster stars. Its rate is controlled by a number low-energy resonances slowly varying non-resonant component. Three new at $E_p$ = 156.2, 189.5, 259.7 keV have recently been confirmed. However, significant uncertainty on reaction remains due to process two suggested 71 105 keV. Here, data with high statistics low...
Context. Material processed by the CNO cycle in stellar interiors is enriched 17O. When mixing processes from surface reach these layers, as occurs when stars become red giants and undergo first dredge up, abundance of 17O increases. Such an occurrence explains drop 16O/17O observed RGB with mass larger than 1.5 M_\solar. As a consequence, interstellar medium continuously polluted wind evolved . Aims. Recently, Laboratory for Underground Nuclear Astrophysics (LUNA) collaboration released...