A5067337480- Nuclear physics research studies
- Gamma-ray bursts and supernovae
- Neutrino Physics Research
- Particle physics theoretical and experimental studies
- Astronomical and nuclear sciences
- Pulsars and Gravitational Waves Research
- Nuclear Physics and Applications
- Atomic and Molecular Physics
- Astrophysics and Cosmic Phenomena
- Astro and Planetary Science
- Quantum Chromodynamics and Particle Interactions
- Advanced Chemical Physics Studies
- Advanced NMR Techniques and Applications
- Nuclear reactor physics and engineering
- Particle accelerators and beam dynamics
- Stellar, planetary, and galactic studies
- Astronomy and Astrophysical Research
- Astrophysical Phenomena and Observations
- Atomic and Subatomic Physics Research
- Quantum, superfluid, helium dynamics
- Scientific Research and Discoveries
- High-Energy Particle Collisions Research
- Cosmology and Gravitation Theories
- Superconducting Materials and Applications
- Dark Matter and Cosmic Phenomena
GSI Helmholtz Centre for Heavy Ion Research
2016-2025
Technical University of Darmstadt
2016-2025
Max Planck Institute for Nuclear Physics
2023
Pioneer (Japan)
2023
LIP - Laboratory of Instrumentation and Experimental Particle Physics
2023
Institut für Hochschulforschung
2023
RIKEN
2023
Heidelberg Institute for Theoretical Studies
2023
Queen's University Belfast
2023
Heidelberg University
2023
The last decade has witnessed both quantitative and qualitative progress in shell-model studies, which have resulted remarkable gains our understanding of the structure nucleus. Indeed, it is now possible to diagonalize matrices determinantal spaces dimensionality up ${10}^{9}$ using Lanczos tridiagonal construction, whose formal numerical aspects are analyzed this review. In addition, many new approximation methods been developed order overcome limitations. New effective nucleon-nucleon...
The most promising astrophysical sources of kHz gravitational waves (GWs) are the inspiral and merger binary neutron star(NS)/black hole systems.Maximizing scientific return a GW detection will require identifying coincident electromagnetic (EM) counterpart.One likely isotropic EM emission from compact object mergers is supernova-like transient powered by radioactive decay heavy elements synthesized in ejecta merger.We present first calculations optical transients that self-consistently...
We present a new nucleosynthesis process that we denote as the nu p process, which occurs in supernovae (and possibly gamma-ray bursts) when strong neutrino fluxes create proton-rich ejecta. In this antineutrino absorptions environment produce neutrons are immediately captured by neutron-deficient nuclei. This allows for of nuclei with mass numbers A>64, , making possible candidate to explain origin solar abundances (92,94)Mo and (96,98)Ru. also offers natural explanation large abundance Sr...
Recent experimental data and progress in nuclear structure modeling have led to improved descriptions of astrophysically important weak-interaction processes. This review discusses these advances their applications hydrostatic solar stellar burning, the slow rapid neutron-capture processes, neutrino nucleosynthesis, explosive hydrogen burning. Special emphasis is given processes associated with core-collapse supernovae. Despite significant progress, improvements are still warranted expected...
The production of about half the heavy elements found in nature is assigned to a specific astrophysical nucleosynthesis process: rapid neutron capture process (r-process). Although this idea has been postulated more than six decades ago, full understanding faces two types uncertainties/open questions: (a) path nuclear chart runs close neutron-drip line, where presently only limited experimental information available, and one rely strongly on theoretical predictions for properties. (b) While...
We present an extensive study of nuclear matrix elements (NME) for the neutrinoless double beta decay nuclei $^{48}$Ca, $^{76}$Ge, $^{82}$Se, $^{96}$Zr, $^{100}$Mo, $^{116}$Cd, $^{124}$Sn, $^{128}$Te, $^{130}$Te, $^{136}$Xe, and $^{150}$Nd based on state-of-the-art energy density functional methods using Gogny D1S functional. Beyond mean-field effects are included within generating coordinate method with particle number angular momentum projection both initial final ground states. obtain a...
Background: $r$-process nucleosynthesis models rely, by necessity, on nuclear structure for input. Particularly important are $\ensuremath{\beta}$-decay half-lives of neutron-rich nuclei. At present only a single systematic calculation exists that provides values all relevant nuclei making it difficult to test the sensitivity this Additionally, even though there indications their contribution may be significant, impact first-forbidden transitions decay rates has not been systematically...
The most efficient axion production mechanism in a supernova (SN) core is the nucleon-nucleon bremsstrahlung. This process has been often modeled at level of vacuum one-pion exchange (OPE) approximation. Starting from this naive recipe, we revise calculation including systematically different effects, namely non-vanishing mass for exchanged pion, contribution two-pions exchange, effective in-medium nucleon masses and multiple scatterings. Moreover, allow an arbitrary degree degeneracy. A...
We implement a multi-group and discrete-ordinate neutrino transport model in spherical symmetry which allows to simulate collective oscillations by including realistic collisional rates self-consistent way. utilize this innovative model, based on strategic parameter rescaling, study recently proposed flavor instability caused the asymmetry of emission absorption between $\nu_e$ $\bar\nu_e$ for four different static backgrounds taken from stages core-collapse supernova simulation. Our results...
Supernova simulations to date have assumed that during core collapse electron captures occur dominantly on free protons, while heavy nuclei are Pauli blocked and ignored. We calculated rates for capture with mass numbers A=65-112 the temperatures densities appropriate collapse. find these large enough so that, in contrast previous assumptions, dominates over protons. This leads significant changes simulations.
Exact diagonalizations with a minimally modified realistic force lead to detailed agreement measured level schemes and electromagnetic transitions in $^{48}$Ca, $^{48}$Sc, $^{48}$Ti, $^{48}$V, $^{48}$Cr $^{48}$Mn. Gamow-Teller strength functions are systematically calculated reproduce the data within standard quenching factor. Their fine structure indicates that fragmentation makes much unobservable. As by-product, calculations suggest microscopic description of onset rotational motion. The...
We have calculated the Gamow-Teller matrix elements of 64 decays nuclei in mass range $A=41\ensuremath{-}50$. In all cases valence space full $\mathrm{pf}$ shell is used. Agreement with experimental results demands introduction an average quenching factor $q=0.744\ifmmode\pm\else\textpm\fi{}0.015$ slightly smaller but statistically compatible $\mathrm{sd}$-shell value, thus indicating that present number close to limit for large $A$.
The most important weak nuclear interaction to the dynamics of stellar core collapse is electron capture, primarily on nuclei with masses larger than 60. In prior simulations collapse, capture these has been treated in a highly parametrized fashion, if not ignored. With realistic treatment heavy come significant changes hydrodynamics and bounce. We discuss as well ramifications for postbounce evolution supernovae.
With currently known input physics and computer simulations in one dimension, a self-consistent treatment of core-collapse supernovae does not yet lead to successful explosions, while two-dimensional models show some promise. Thus, there are strong indications that the delayed neutrino mechanism works combined with multidimensional convection for unstable layers (possibly aid rotation, magnetic fields and/or still existent uncertainties opacities). On other hand, is need provide correct...
Recent shell-model calculations of weak-interaction rates for nuclei in the mass range A = 45-65 have resulted substantial revisions to hitherto standard set Fuller, Fowler, & Newman (FFN). In particular, key electron-capture rates, such as that 60Co, are much smaller. We consider here effects these revised on presupernova (post-oxygen burning) evolution massive stars 11-40 M☉. Moreover, we include, first time models by our group, modern beta decay addition electron capture and positron...
We perform three-flavor Boltzmann neutrino transport radiation hydrodynamics simulations covering a period of 3 s after the formation protoneutron star in core-collapse supernova explosion. Our results show that treatment charged-current interactions hot and dense matter as suggested by Reddy et al. [Phys. Rev. D 58, 013009 (1998)] has strong impact on luminosities spectra emitted neutrinos. When compared with neglect mean-field effects opacities, we find all flavors are reduced while...
The stellar mass range 8 ≲ M/M☉ 12 corresponds to the most massive asymptotic giant branch (AGB) stars and numerous stars. It is host a variety of supernova (SN) progenitors therefore very important for galactic chemical evolution population studies. In this paper, we study transition from super-AGB (SAGB) star find that propagating neon–oxygen-burning shell common both electron capture (EC-SN) lowest iron-core-collapse (FeCCSN) progenitors. Of models ignite neon-burning off-center, 9.5 M☉...
The nuclear structure in regions of the Segré chart which are astrophysical importance is reviewed. main emphasis put on those nuclei that relevant for stellar nucleosynthesis fusion processes, and slow neutron capture, both located close to stability, rapid capture dripline proton near dripline. basic features modern structure, their future potential astrophysics level predictibility critically discussed. Recent experimental theoretical results shell evolution far off stability line...
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),...