A5101623891- Nuclear physics research studies
- Quantum Chromodynamics and Particle Interactions
- Particle physics theoretical and experimental studies
- High-Energy Particle Collisions Research
- Nuclear Physics and Applications
- Astronomical and nuclear sciences
- Nuclear reactor physics and engineering
- Atomic and Molecular Physics
- Advanced Chemical Physics Studies
- X-ray Spectroscopy and Fluorescence Analysis
- Magnetic confinement fusion research
- Superconducting Materials and Applications
- Radiation Detection and Scintillator Technologies
- Neutrino Physics Research
- Advanced NMR Techniques and Applications
- Fusion materials and technologies
- Particle Detector Development and Performance
- Radiopharmaceutical Chemistry and Applications
- Organometallic Complex Synthesis and Catalysis
- Catalytic Processes in Materials Science
- Catalysts for Methane Reforming
- Astro and Planetary Science
- Electron and X-Ray Spectroscopy Techniques
- Electrocatalysts for Energy Conversion
- Hydrogen Storage and Materials
HUN-REN Institute for Nuclear Research
2015-2024
University of Debrecen
1996-2024
Budapest University of Technology and Economics
2006-2024
Wageningen University & Research
2024
RIKEN Nishina Center
2016-2023
RIKEN
2022-2023
Eötvös Loránd University
1988-2022
Hungarian Research Network
2022
Hungarian Academy of Sciences
2011-2021
ExxonMobil (United States)
1999-2021
The hydroformylation of decene-1 was studied in the presence fluorous-soluble P[CH2CH2(CF2)5CF3]3 modified rhodium catalyst at 100 °C and 1.1 MPa CO/H2 (1:1) a 50/50 vol % toluene/C6F11CF3 solvent mixture, which forms homogeneous liquid phase above °C. selected on basis semiempirical calculation electronic properties P[(CH2)x(CF2)yCF3]3 (x = 0, y 2, 4 x 0−5, 2) prepared by reaction PH3 with CH2CH(CF2)5CF3. solution structure HRh(CO){P[CH2CH2(CF2)5CF3]3}3 (1) C6F11CF3 is similar to that...
Based on semiempirical quantum-chemical calculations, the electronic band structure of β-Ga2O3 is presented and formation properties oxygen vacancies are analyzed. The equilibrium geometries energies neutral doubly ionized were calculated. Using calculated donor level positions vacancies, high temperature n-type conduction explained. vacancy concentration obtained by fitting to experimental resistivity electron mobility.
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,...
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...
In an experiment with the BigRIPS separator at RIKEN Nishina Center, we observed two-proton (2p) emission from ^{67}Kr. At same time, no evidence for 2p of ^{59}Ge and ^{63}Se, two other potential candidates this exotic radioactivity, could be observed. This observation is in line Q value predictions which pointed to ^{67}Kr as being best new candidate among three radioactivity. only fourth ground-state emitter a half-life order few milliseconds. The decay energy was determined 1690(17) keV,...
Abstract Bei der Bildung des Ascorbigens aus L ‐Ascorbinsäure und 3‐Hydroxymethylindol tritt eine C‐Alkylierung am C‐2 Ascorbat‐Ions ein, wobei sich 2 diastereomere Ascorbigene bilden.
The primary aim of experimental nuclear astrophysics is to determine the rates reactions taking place in stars various astrophysical conditions. These reaction are important ingredient for understanding elemental abundance distribution our solar system and galaxy. determined from cross sections which need be measured at energies as close astrophysically relevant ones possible. In many cases final nucleus an radioactive allows section based on off-line measurement number produced isotopes....
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 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 $^{17}\mathrm{O}$($p,\ensuremath{\alpha}$)$^{14}\mathrm{N}$ 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...
A disruption mitigation system (DMS) is under design for ITER to inject sufficient material deeply into the plasma rapid thermal shutdown and collisional suppression of any resulting runaway electrons. Progress on development both a shattered pellet injector (SPI) that produces large solid cryogenic pellets provide reliable deep penetration fast opening high flow rate gas valve massive injection (MGI) presented. Cryogenic deuterium neon up 25 mm in size have been formed accelerated with...
ADVERTISEMENT RETURN TO ISSUEPREVArticleNEXTDihydrogen: a better ligand than water? IR and x-ray evidence for aquo coordination in W(CO)3(PR3)2(H2O), thermodynamics of H2O binding versus .eta.2-H2 H2O/D2 isotopic exchange. Implications the biological activation hydrogenGregroy J. Kubas, Carol Burns, Guru Rattan K. Khalsa, Lori Stepan Van Der Sluys, Gabor Kiss, Carl D. HoffCite this: Organometallics 1992, 11, 10, 3390–3404Publication Date (Print):October 1, 1992Publication History Published...
The $^{106}\mathrm{Cd}$($\ensuremath{\alpha},\ensuremath{\gamma})$$^{110}\mathrm{Sn}$ reaction cross section has been measured in the energy range of Gamow window for astrophysical $p$-process scenario. sections $^{106}\mathrm{Cd}$($\ensuremath{\alpha},n$)$^{109}\mathrm{Sn}$ and $^{106}\mathrm{Cd}$($\ensuremath{\alpha},p$)$^{109}\mathrm{In}$ below ($\ensuremath{\alpha},n$) threshold have also determined. results are compared with predictions statistical model code NON-SMOKER using different...
The $^{18}\mathrm{O}(p,\ensuremath{\alpha})^{15}\mathrm{N}$ reaction is of primary importance in several astrophysical scenarios, including fluorine nucleosynthesis inside asymptotic giant branch stars as well oxygen and nitrogen isotopic ratios meteorite grains. Thus the indirect measurement low energy region has been performed to reduce nuclear uncertainty on theoretical predictions. In particular strength 20 90 keV resonances deduced change rate evaluated.
A new measurement of the 11B(p,?0)8Be has been performed applying Trojan horse method (THM) to 2H(11B,?80Be)n quasi-free reaction induced at a laboratory energy 27 MeV. The astrophysical S(E) factor extracted from ?600 keV down zero by means an improved data analysis technique and it compared with direct available in literature. range investigated here overlaps region light element LiBeB stellar burning that future aneutronic fusion power plants using 11B+p fuel cycle. investigation...
The Trojan horse nucleus invariance for the binary reaction cross section extracted from was tested using quasifree $^{3}\mathrm{He}$($^{6}\mathrm{Li}$,$\ensuremath{\alpha}\ensuremath{\alpha}$)H and $^{3}\mathrm{He}$($^{7}\mathrm{Li}$,$\ensuremath{\alpha}\ensuremath{\alpha}$)$^{2}\mathrm{H}$ reactions. sections $^{6}\mathrm{Li}$($d$,$\ensuremath{\alpha}){}^{4}$He $^{7}\mathrm{Li}$($p$,$\ensuremath{\alpha}){}^{4}$He processes were in framework of plane wave approximation. They are compared...
The (13)C(α,n)(16)O reaction is the neutron source for main component of s-process, responsible production most nuclei in mass range 90</~A</~204. It active inside helium-burning shell asymptotic giant branch stars, at temperatures </~10(8) K, corresponding to an energy interval where effective from 140 230 keV. In this region, astrophysical S(E)-factor dominated by -3 keV subthreshold resonance due 6.356 MeV level (17)O, giving rise a steep increase S(E)-factor. Notwithstanding that it...