G. F. Ciani
A5024631937- Nuclear physics research studies
- Nuclear Physics and Applications
- Astronomical and nuclear sciences
- Astro and Planetary Science
- Nuclear reactor physics and engineering
- Stellar, planetary, and galactic studies
- Gamma-ray bursts and supernovae
- Particle physics theoretical and experimental studies
- Atomic and Molecular Physics
- Radiation Detection and Scintillator Technologies
- Neutrino Physics Research
- X-ray Spectroscopy and Fluorescence Analysis
- Atomic and Subatomic Physics Research
- Radiation Therapy and Dosimetry
- Quantum Chromodynamics and Particle Interactions
- Algorithms and Data Compression
- Spectroscopy and Laser Applications
- Pulsars and Gravitational Waves Research
- High-Energy Particle Collisions Research
- Astrophysics and Cosmic Phenomena
- Quantum, superfluid, helium dynamics
- Advanced NMR Techniques and Applications
- Superconducting Materials and Applications
- Astrophysics and Star Formation Studies
- Atmospheric Ozone and Climate
Istituto Nazionale di Fisica Nucleare, Sezione di Bari
2021-2025
University of Bari Aldo Moro
2016-2024
Gran Sasso Science Institute
2016-2022
University of Campania "Luigi Vanvitelli"
2021-2022
Istituto Nazionale di Fisica Nucleare, Laboratori Nazionali del Gran Sasso
2016-2021
Istituto Nazionale di Fisica Nucleare
2019-2021
HUN-REN Institute for Nuclear Research
2020-2021
Hungarian Academy of Sciences
2020
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...
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 Particle identification techniques are fundamental tools in nuclear physics experiments. Discriminating particles or nuclei produced interactions allows to better understand the underlying mechanisms. The energy interval of these reactions is very broad, from sub-eV up TeV. For this reason, many different approaches have been developed, often combining two more observables. This paper reviews several with emphasis on expertise gained within current scientific program Italian...
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...
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...
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 NeNa and the MgAl cycles play a fundamental role in nucleosynthesis of asymptotic giant branch stars undergoing hot bottom burning. Na23(p,γ)24Mg reaction links these two precise determination its rate is required to correctly estimate contribution chemical evolution various isotopes Na, Mg Al. At temperatures 50≲T≲110MK, narrow resonances at Ep=140 251keV are main contributors rate, addition direct capture that dominates lower part temperature range. We present new measurements...
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...
Low mass Asymptotic Giant Branch stars are among the most important polluters of interstellar medium. In their interiors, main component (A>90) slow neutron capture process (the s-process) is synthesized, source being 13C(alpha,n)16O reaction. this paper we review its current experimental status discussing possible future synergies between some experiments currently focused on determination rate. Moreover, in order to determine level precision needed fully characterize reaction, present a...