A5080769390- Nuclear physics research studies
- Nuclear Physics and Applications
- Nuclear reactor physics and engineering
- Astronomical and nuclear sciences
- Gamma-ray bursts and supernovae
- Astro and Planetary Science
- Radiation Detection and Scintillator Technologies
- Stellar, planetary, and galactic studies
- Atomic and Molecular Physics
- Advanced Chemical Physics Studies
- Atomic and Subatomic Physics Research
- Particle physics theoretical and experimental studies
- Nuclear Materials and Properties
- Quantum Chromodynamics and Particle Interactions
- Scientific Research and Discoveries
- Corporate Governance and Law
- Superconducting Materials and Applications
- European and International Law Studies
- Conflict of Laws and Jurisdiction
- Astronomy and Astrophysical Research
- Radiation Therapy and Dosimetry
- Particle Detector Development and Performance
- Neutrino Physics Research
- Law and Political Science
- European and International Contract Law
Fraunhofer Institute for Manufacturing Technology and Advanced Materials
2020-2025
Medizinische Hochschule Hannover
2025
University of Basel
2015-2024
University of Hertfordshire
2015-2024
Charles University
2009-2023
Bhabha Atomic Research Centre
2023
European Organization for Nuclear Research
2014-2021
Commissariat à l'Énergie Atomique et aux Énergies Alternatives
2007-2020
CEA DAM Île-de-France
2020
TU Dresden
2014-2019
We present results from the JINA REACLIB project, an ongoing effort to maintain a current and accurate library of thermonuclear reaction rates for astrophysical applications. Ongoing updates are transparently documented version tracked, any set is publicly available can be downloaded via Web interface at http://groups.nscl.msu.edu/jina/reaclib/db/. discuss here our V1.0, snapshot recommended stable explosive hydrogen helium burning. show that updated lead modest but significant changes in...
We present the first calculations to follow evolution of all stable nuclei and their radioactive progenitors in stellar models computed from onset central hydrogen burning through explosion as Type II supernovae. Calculations are performed for Pop I stars 15, 19, 20, 21, 25 M_sun using most recently available experimental theoretical nuclear data, revised opacity tables, neutrino losses, weak interaction rates, taking into account mass loss due winds. A novel ``adaptive'' reaction network is...
We present nuclear reaction network calculations to investigate the influence of structure on rp-process between Ge and Sn in various scenarios. Due lack experimental data for neutron-deficient nuclei this region, we discuss currently available model predictions masses deformations as well methods calculating rates (Hauser-Feshbach) β-decay (QRPA shell model). In addition, apply a valence nucleon (NpNn) correlation scheme prediction deformations. also describe 2p-capture reactions, which had...
We calculate the rapid proton ( rp) capture process of hydrogen burning on surface an accreting neutron star with updated reaction network that extends up to Xe, far beyond previous work. In both steady-state nuclear appropriate for rapidly stars (such as magnetic polar caps x-ray pulsars) and unstable type I bursts, we find rp ends in a closed SnSbTe cycle. This prevents synthesis elements heavier than Te has important consequences burst profiles, composition stars, potentially galactic...
The neutron time-of-flight facility n_TOF features a white source produced by spallation through 20GeV/c protons impinging on lead target. facility, aiming primarily at the measurement of neutron-induced reaction cross sections, was operating CERN between 2001 and 2004, then underwent major upgrade in 2008. This paper presents detail all characteristics new beam currently available configurations, which correspond to two different collimation systems choices moderator. discussed include...
Rotation was shown to have a strong impact on the structure and light element nucleosynthesis in massive stars. In particular, models including rotation can reproduce primary nitrogen observed halo extremely metal-poor (EMP) Additional exploratory showed that may enhance $s$-process production at low metallicity. Here we present large grid of star full network study weak $s$-process. We explore possibility producing significant amounts elements beyond strontium peak, which is where usually...
Axionlike particles (ALPs) coupled to nucleons might be copiously emitted from a supernova (SN) core. We extend existing bounds on free-streaming ALPs the case in which these are so strongly interacting with nuclear matter trapped SN For ALPs, we also bound absence of an ALP-induced signal Kamiokande-II neutrino detector at time 1987A. find that combining different arguments, SNe exclude values ALP-nucleon coupling <a:math xmlns:a="http://www.w3.org/1998/Math/MathML"...
The prediction of cross sections for nuclei far off stability is crucial in the field nuclear astrophysics. In recent calculations level density---as an important ingredient to statistical model (Hauser-Feshbach)---has shown highest uncertainties. We present a global parametrization densities within back-shifted Fermi-gas formalism. Employment energy-dependent density parameter $a$, based on microscopic corrections from finite range droplet mass formula, and backshift $\ensuremath{\delta}$,...
Multi-zone models of Type I X-ray bursts are presented that use an adaptive nuclear reaction network unprecedented size, up to 1300 isotopes. Sequences 15 followed for two choices accretion rate and metallicity. At 0.1 Eddington (and 0.02 low metallicity), combined hydrogen-helium flashes occur. The rise times, shapes, tails these light curves sensitive the efficiency burning at various waiting points along rp-process path sensitivities explored. show "compositional inertia", in their...
The rapid neutron-capture process (r-process) encounters unstable nuclei far from β-stability. Therefore its observable features, like the abundances, witness (still uncertain) nuclear structure as well conditions in appropriate astrophysical environment. With remaining lack of a full understanding origin, parameterized calculations are still needed. We consider two approaches: (1) classical approach is based on (constant) neutron number densities nn and temperatures T over duration...
The astrophysical site of the r-process is still uncertain, and a full exploration systematics this process in terms its dependence on nuclear properties from stability to neutron drip-line within realistic stellar environments has be undertaken. Sufficiently high seed ratios can only obtained either very neutron-rich low-entropy or moderately high-entropy environments, related star mergers (or jets matter) wind core-collapse supernova explosions. As chemical evolution models seem disfavor...
Comparing observational abundance features with nucleosynthesis predictions of stellar evolution or explosion simulations can scrutinize two aspects: (a) the conditions in astrophysical production site and (b) quality nuclear physics input utilized. We test r-process calculations for dynamical ejecta neutron star merger based on three different mass models: The Finite Range Droplet Model (FRDM), (quenched version the) Extended Thomas Fermi Strutinsky Integral (ETFSI-Q),...
A small number of naturally occurring, proton-rich nuclides (the p-nuclei) cannot be made in the s- and r-processes. Their origin is not well understood. Massive stars can produce p-nuclei through photodisintegration pre-existing intermediate heavy nuclei. This so-called γ-process requires high stellar plasma temperatures occurs mainly explosive O/Ne burning during a core-collapse supernova. Although massive has been successful producing large range p-nuclei, significant deficiencies remain....
Axions coupled to nucleons might be copiously emitted from core-collapse supernovae (SNe). If the axion-nucleon coupling is strong enough, then axions would SN as a burst and, reaching Earth, may excite oxygen nuclei in water \ifmmode \check{C}\else \v{C}\fi{}herenkov detectors ($^{16}\mathrm{O}+a\ensuremath{\rightarrow}^{16}\mathrm{O}^{*}$). This process will followed by decay(s) of excited state resulting an emission photons and thus providing possibility for direct detection galactic...
view Abstract Citations (134) References (122) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Production of Heavy Elements in Inhomogeneous Cosmologies Rauscher, Thomas ; Applegate, James H. Cowan, John J. Thielemann, Friedrich-Karl Wiescher, Michael Baryon density inhomogeneities during big bang nucleosynthesis can result from a variety possible causes (e.g., quantum chromodynamic and electroweak phase transitions; cosmic strings). We present here the...
The masses of very neutron-deficient nuclides close to the astrophysical rp- and νp-process paths have been determined with Penning trap facilities JYFLTRAP at JYFL/Jyväskylä SHIPTRAP GSI/Darmstadt. Isotopes from yttrium (Z=39) palladium (Z=46) produced in heavy-ion fusion-evaporation reactions. In total, 21 were studied, almost half mass values experimentally for first time: 88Tc, 90−92Ru, 92−94Rh, 94,95Pd. For 95Pdm, (21/2+) high-spin state, a direct determination was performed. Relative...
The location of the ($\ensuremath{\gamma},p)/(\ensuremath{\gamma},n$) and ($\ensuremath{\gamma},\ensuremath{\alpha})/(\ensuremath{\gamma},n$) line at \ensuremath{\gamma} process temperatures is discussed, using updated reaction rates based on global Hauser-Feshbach calculations. results can be directly compared with classic discussions. nuclei exhibiting largest sensitivity to uncertainties in nuclear structure parameters are specified, suggestions for experiments made. Additionally, effect...
Effective energy windows (Gamow windows) of astrophysical reaction rates for ($p,\ensuremath{\gamma}$), ($p,n$), ($p,\ensuremath{\alpha}$), ($\ensuremath{\alpha},\ensuremath{\gamma}$), ($\ensuremath{\alpha},n$), ($\ensuremath{\alpha},p$), ($n,\ensuremath{\gamma}$), ($n,p$), and ($n,\ensuremath{\alpha}$) on targets with $10\ensuremath{\leqslant}Z\ensuremath{\leqslant}83$ from proton to neutron dripline are calculated using theoretical cross sections. It is shown that widely used approximation...
We explore explosions of massive stars, which are triggered via the quark–hadron phase transition during early post-bounce core-collapse supernovae. construct a quark equation state, based on bag model for strange matter. The between hadronic and phases is constructed applying Gibbs conditions. resulting hybrid equations state used in supernova simulations, general relativistic radiation hydrodynamics three-flavor Boltzmann neutrino transport spherical symmetry. formation mixed reduces...
Among extinct radioactivities present in meteorites, 60Fe (t1/2 = 1.49 Myr) plays a key role as high-resolution chronometer, heat source planetesimals, and fingerprint of the astrophysical setting solar system formation. A critical issue with is that it could have been heterogeneously distributed protoplanetary disk, calling into question efficiency mixing nebula or timing injection relative to planetesimal If this were case, one would expect meteorites did not incorporate (either because...
Sensitivities of nuclear reaction rates to a variation properties are studied. Target nuclei range from proton- neutron dripline for 10 ⩽ Z 83. Reactions considered nucleon- and α-induced reactions mediated by strong interaction. The contribution occurring on the target ground state total stellar rate is also given. General dependencies various input quantities discussed. Additionally, sensitivities laboratory cross-sections nucleon-, α-, γ-induced shown, allowing us estimate impact...