G. Gervino
A5000825822- Nuclear physics research studies
- Nuclear Physics and Applications
- Particle physics theoretical and experimental studies
- Quantum Chromodynamics and Particle Interactions
- Radiation Detection and Scintillator Technologies
- High-Energy Particle Collisions Research
- Atomic and Subatomic Physics Research
- Astronomical and nuclear sciences
- Neutrino Physics Research
- Nuclear reactor physics and engineering
- Atomic and Molecular Physics
- Quantum, superfluid, helium dynamics
- Gamma-ray bursts and supernovae
- Dark Matter and Cosmic Phenomena
- Particle Detector Development and Performance
- Superconducting Materials and Applications
- Statistical Mechanics and Entropy
- Astro and Planetary Science
- Radioactivity and Radon Measurements
- Radiation Therapy and Dosimetry
- Particle Accelerators and Free-Electron Lasers
- Medical Imaging Techniques and Applications
- Advanced Chemical Physics Studies
- Earthquake Detection and Analysis
- Stellar, planetary, and galactic studies
Istituto Nazionale di Fisica Nucleare, Sezione di Torino
2016-2025
University of Turin
2016-2025
Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas
2024
Istituto Nazionale di Fisica Nucleare
1986-2024
Instituto de Física Corpuscular
2024
Universitat de València
2024
University of Edinburgh
2021
Gran Sasso Science Institute
2019
Istituto Nazionale di Fisica Nucleare, Laboratori Nazionali del Gran Sasso
2019
Polytechnic University of Turin
1996-2018
We report on a new measurement of the 14N(p,γ)15O capture cross section at Ep=140 to 400 keV using kV LUNA accelerator facility Laboratori Nazionali del Gran Sasso (LNGS). The uncertainties have been reduced with respect previous measurements and their analysis. analyzed data R-matrix method we find that ground state transition accounts for about 15% total S-factor. main contribution S-factor is given by 6.79 MeV state. S(0)=1.7±0.2 b, in agreement recent extrapolations. result has important...
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...
We give the LUNA results on cross section measurement of a key reaction proton-proton chain strongly affecting calculated neutrino luminosity from Sun: He3+He3-->He4+2p. Due to cosmic ray suppression provided by Gran Sasso underground laboratory it has been possible measure down lower edge solar Gamow peak, i.e. as low 16.5 keV centre mass energy. The data clearly show increase due electron screening effect but they do not exhibit any evidence for narrow resonance suggested explain observed flux.
The transition between the Main Sequence and Red Giant Branch in low mass stars is powered by onset of CNO burning, whose bottleneck 14N(p, O. LUNA collaboration has recently improved energy measurements cross section this key reaction. We analyse impact revised reaction rate on estimate Globular Cluster ages, as derived from turnoff luminosity. found that age oldest Clusters should be increased about 0.7-1 Gyr with respect to current estimates.
The nuclear physics input from the He3(α,γ)Be7 cross section is a major uncertainty in fluxes of Be7 and B8 neutrinos Sun predicted by solar models Li7 abundance obtained big-bang nucleosynthesis calculations. present work reports on new precision experiment using activation technique at energies directly relevant to nucleosynthesis. Previously such low had been reached experimentally only prompt-γ with inferior precision. Using windowless gas target, high beam intensity, background...
Solar neutrino fluxes depend both on astrophysical and nuclear physics inputs, namely the cross sections of reactions responsible for production inside core. While flux solar $^{8}\mathrm{B}$ neutrinos has been recently measured at Superkamiokande with a 3.5% uncertainty precise measurement $^{7}\mathrm{Be}$ is foreseen in next future, predicted are still affected by larger errors. The largest to determine comes from...
In stars with temperatures above 20×106K, hydrogen burning is dominated by the CNO cycle. Its rate determined slowest process, 14N(p, γ)15O reaction. Deep underground in Italy's Gran Sasso laboratory, at LUNA 400 kV accelerator, cross section of this reaction has been measured energies much lower than ever achieved before. Using a windowless gas target and 4π BGO summing detector, direct data obtained down to 70 keV, reaching value 0.24 picobarn. The Gamow peak covered experimental for...
New results on quasi-free η photoproduction the neutron and proton bound in a deuteron target are presented. The γn→ηn cross section reveals bump-like structure which is not seen proton. This may signal existence of relatively narrow (M∼1.68GeV, Γ⩽30MeV) baryon state.
Abstract We investigate the relativistic equation of state hadronic matter and quark-gluon plasma at finite temperature baryon density in framework non-extensive statistical mechanics, characterized by power-law quantum distributions. impose Gibbs conditions on global conservation number, electric charge strangeness number. For phase, we study an extended mean-field theoretical model with inclusion strange particles (hyperons mesons). quark sector, employ MIT-Bag model. In this context focus...
To date, the effects of electromagnetic fields on cell metabolism have been overlooked. The objective present study was to investigate influence extremely low frequency (ELF-EMF) over mitochondrial and consequent impact cancer growth.The ELF-EMF growth were investigated in several human lines by crystal violet assay. modulation activity assessed cytofluorimetric evaluation membrane potential real-time quantification transcription. Moreover expression proteins their levels organelle...
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...
We present new $\ensuremath{\Sigma}$ beam asymmetry data for $\ensuremath{\eta}$ meson photoproduction on the proton, using a novel tagged, laser backscattered, linearly polarized photon up to 1.1 GeV. The show large, positive asymmetries, at all incident energies. In addition ${S}_{11}(1535)$ and ${D}_{13}(1520)$ resonances necessary reproduce cross sections, ${P}_{13}(1720)$ ${D}_{15}(1675)$ ``four stars'' contribute observable, but cannot strong forward asymmetries measured energies...
We report on the results of ${}^{3}\mathrm{He}{(}^{4}\mathrm{He}{,2p)}^{4}\mathrm{He}$ experiment at underground accelerator facility LUNA (Gran Sasso). For first time lowest projectile energies utilized for cross section measurement correspond to below center solar Gamow peak ${(E}_{0}=22 \mathrm{keV})$. The data provide no evidence existence a hypothetical resonance in energy range investigated. Although extrapolation is needed anymore (except low-energy tail peak), must be corrected...