A5014920343- Nuclear physics research studies
- Nuclear Physics and Applications
- Astronomical and nuclear sciences
- Quantum Chromodynamics and Particle Interactions
- Atomic and Molecular Physics
- Particle physics theoretical and experimental studies
- Nuclear reactor physics and engineering
- Advanced Chemical Physics Studies
- X-ray Spectroscopy and Fluorescence Analysis
- Astro and Planetary Science
- Gamma-ray bursts and supernovae
- Radiopharmaceutical Chemistry and Applications
- Boron Compounds in Chemistry
- Medical Imaging Techniques and Applications
- Advanced NMR Techniques and Applications
- Stellar, planetary, and galactic studies
- Radiation Therapy and Dosimetry
- Neutrino Physics Research
- Superconducting Materials and Applications
- Particle accelerators and beam dynamics
- Quantum, superfluid, helium dynamics
- Inorganic Fluorides and Related Compounds
- Scientific Research and Discoveries
- Electron and X-Ray Spectroscopy Techniques
- Atomic and Subatomic Physics Research
University of Catania
2016-2025
Istituto Nazionale di Fisica Nucleare, Laboratori Nazionali del Sud
2015-2024
Istituto Nazionale di Fisica Nucleare
2012-2024
Centro Siciliano di Fisica Nucleare e di Struttura della Materia
2004-2024
Osservatorio Astrofisico di Catania
2020-2023
Istituto Nazionale di Fisica Nucleare, Sezione di Napoli
2009-2020
Texas A&M University – Commerce
2009-2019
Università degli Studi di Enna Kore
2009-2019
Beijing Normal University
2015-2017
Beijing Radiation Center
2015-2017
Nuclear reaction rates are among the most important input for understanding primordial nucleosynthesis and therefore a quantitative description of early Universe. An up-to-date compilation direct cross sections 2H(d,p)3H, 2H(d,n)3He, 7Li(p,alpha)4He 3He(d,p)4He reactions is given. These uncertain used Big Bang calculations. Their measurements through Trojan Horse Method (THM) also reviewed compared with data. The corresponding recommended errors in this work were as calculations to evaluate...
The 19F(p, α)16O reaction is an important fluorine destruction channel in the proton-rich outer layers of asymptotic giant branch (AGB) stars and it might also play a role hydrogen-deficient post-AGB star nucleosynthesis. So far, available direct measurements do not reach energy region astrophysical interest (Ecm ≲ 300 keV), because hindrance effect Coulomb barrier. Trojan Horse (TH) method was thus used to access this region, by extracting quasi-free contribution 2H(19F, α16O)n 19F(3He,...
The decay path of the Hoyle state in 12C (Ex=7.654 MeV) has been studied with 14N(d,α2)12C(7.654) reaction induced at 10.5 MeV. High resolution invariant mass spectroscopy techniques have allowed us to unambiguously disentangle direct and sequential decays passing through ground 8Be. Thanks almost total absence background attained resolution, a fully contribution width observed. is negligible, an upper limit 0.043% (95% C.L.). precision this result about factor 5 higher than previous...
Measurement of nuclear cross sections at astrophysical energies involving unstable species is one the most challenging tasks in experimental physics. The use indirect methods often unavoidable this scenario. In paper Trojan horse method applied for first time to a radioactive ion beam-induced reaction studying ${}^{18}\mathrm{F}(p,\ensuremath{\alpha}$)${}^{15}\mathrm{O}$ process low relevant astrophysics via three-body...
The cross sections of the 2H(d,p)3H and 2H(d,n)3He reactions have been measured via Trojan Horse method applied to quasi-free 2H(3He,p3H)1H 2H(3He,n3He)1H processes at 18 MeV off proton in 3He. For first time, bare nucleus S(E) factors determined from 1.5 MeV, across relevant region for standard Big Bang nucleosynthesis, down thermal energies deuterium burning pre-main-sequence (PMS) phase stellar evolution, as well future fusion reactors. Both energy dependence absolute value deviate by...
Abstract Fluorine abundance determination is of great importance in stellar physics to understand s-elements production and mixing processes asymptotic giant branch (AGB) stars. Up now, theoretical models overproduce F abundances AGB stars with respect the observed values, thus calling for further investigation reactions involving fluorine. In particular, 19 F( p , α ) 16 O reaction main destruction channel fluorine at bottom convective envelope stars, an H-rich environment where it can...
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....
The Trojan Horse Method (THM) represents an indirect path to determine the bare nucleus astrophysical S-factor for reactions among charged particles at energies. This is achieved by measuring quasi-free cross section of a suitable three-body process. method also suited study neutron-induced reactions, especially in case radioactive ion beams. A comprehensive review theoretical as well experimental features behind THM presented here. An overview given some recent applications demonstrate...
High power lasers have proven being capable to produce high energy gamma rays, charged particles and neutrons induce all kinds of nuclear reactions. At ELI, the studies with will enter for first time into new domains intensities.
Abstract Nuclear astrophysics is a field at the intersection of nuclear physics and astrophysics, which seeks to understand engines astronomical objects origin chemical elements. This white paper summarizes progress status field, new open questions that have emerged, tremendous scientific opportunities opened up with major advances in capabilities across an ever growing number disciplines subfields need be integrated. We take holistic view discussing unique challenges regards science,...
The $^{11}\mathrm{B}(p,{\ensuremath{\alpha}}_{0})^{8}\mathrm{Be}$ reaction was studied from $1\phantom{\rule{0.3em}{0ex}}\text{MeV}$ down to astrophysical energies by means of the Trojan-horse method applied $^{2}\mathrm{H}(^{11}\mathrm{B},{\ensuremath{\alpha}}_{o}^{8}\mathrm{Be})n$ three-body performed at an incident energy $27\phantom{\rule{0.3em}{0ex}}\text{MeV}$. Coincidence spectra measured in a kinematically complete experiment show presence quasifree...
The 18O(p, α)15N reaction is of primary importance to pin down the uncertainties, due nuclear physics input, affecting present-day models asymptotic giant branch stars. Its rate can modify both fluorine nucleosynthesis inside such stars and oxygen nitrogen isotopic ratios, which allow one constrain proposed astrophysical scenarios. Thus, an indirect measurement low-energy region has been performed access, for first time, range relevance application. In particular, a full, high-accuracy...
The lithium problem influencing primordial and stellar nucleosynthesis is one of the most interesting unsolved issues in astrophysics. 6Li fragile lithium's stable isotopes largely destroyed stars during pre-main-sequence (PMS) phase. For these stars, convective envelope easily reaches, at least its bottom, relatively low ignition temperature. Thus, gaining an understanding depletion also gives hints about extent regions. this reason, charged-particle-induced reactions have been subject...
The $^{17}\mathrm{O}$($p,\ensuremath{\alpha}$)$^{14}\mathrm{N}$ reaction is of fundamental relevance in several astrophysical scenarios, such as novae, asymptotic giant branch nucleosynthesis, and $\ensuremath{\gamma}$-ray astronomy. We report on the indirect measurement bare-nucleus cross section low-energy region. In particular, two resonances at ${E}_{R}^{\mathrm{c}.\mathrm{m}.}=65$ keV ${E}_{R}^{\mathrm{c}.\mathrm{m}.}=183$ keV, which dominate rate inside Gamow window, have been...
The 13C(α, n)16O reaction is the neutron source for main component of s-process, responsible production most nuclei in mass range 90 ≲ A 208. This takes place inside helium-burning shell asymptotic giant branch stars, at temperatures 108 K, corresponding to an energy interval where effective 140–230 keV. In this regime, astrophysical S(E)-factor dominated by −3 keV sub-threshold resonance due 6.356 MeV level 17O, giving rise a steep increase S-factor. Its contribution still controversial as...
Context. The charged-particle induced reactions on lithium have been studied by several works. In particular, direct measurements of the 7Li(p, α)4He reaction performed to extrapolate its low-energy astrophysical S(E)-factor and evaluate electron screening potential, Ue.
The Trojan horse method allows one to extract the cross section of a binary reaction by properly selecting quasi-free component suitable surrogate reaction. A crucial point its application is discrimination contribution total yield, requiring study experimental momentum distribution adopted nucleus. Deuteron has been largely used as nucleus in $p$- and $n$-induced reactions extracted compared with square Hulth\'en wave function space, which accounts for $s$-wave deuteron function. Here,...
The reaction ${}^{17}\mathrm{O}(n,\ensuremath{\alpha}){}^{14}\mathrm{C}$ was studied at energies from ${E}_{\mathrm{c}.\mathrm{m}.}=0$ to ${E}_{\mathrm{c}.\mathrm{m}.}=350\phantom{\rule{0.28em}{0ex}}\mathrm{keV}$ by using the quasifree deuteron breakup in three-body ${}^{17}\mathrm{O}+d\ensuremath{\rightarrow}\ensuremath{\alpha}+{}^{14}\mathrm{C}+p$, which extended Trojan Horse indirect method (THM) neutron-induced reactions. It is found that ${}^{18}\mathrm{O}$ excited state...
The $^{10}\mathrm{B}(p,{\ensuremath{\alpha}}_{0})^{7}\mathrm{Be}$ bare nucleus astrophysical $S(E)$ factor has been measured for the first time at energies from about 100 keV down to 5 by means of Trojan Horse method (THM). In this energy region, is strongly dominated 8.699 MeV $^{11}\mathrm{C}$ level (${J}^{\ensuremath{\pi}}={\frac{5}{2}}^{+}$), producing an $s$-wave resonance centered 10 in entrance channel. Up now, only high--energy tail measured, while low-energy trend extrapolated...
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...
The $^{3}\mathrm{He}$($d,p$)$^{4}\mathrm{He}$ reaction has been studied from ${E}_{c.m.}=600$ keV down to astrophysical energies by means of the ``Trojan horse'' method using $^{6}\mathrm{Li}$($^{3}\mathrm{He}$,$p\ensuremath{\alpha}$)$^{4}\mathrm{He}$ three-body at ${E}_{\mathrm{lab}}=5$ and 6 MeV. Coincidence spectra were measured in kinematic conditions favoring quasifree $^{3}\mathrm{He}+^{2}\mathrm{H}$ process. bare factor ${S}_{b}(E)$ for was extracted cross section modified plane-wave...