-
Alberto Mengoni (ENEA & INFN, Bologna), Sean John Freeman (CERN)05/09/2022, 09:00
-
Pippa Wells (CERN)05/09/2022, 09:10Invited
-
Urs Wiedemann (CERN)05/09/2022, 09:30Invited
From n_TOF and ISOLDE up to the LHC experiments, a remarkable common denominator of all CERN physics programmes is their interplay with central questions in astrophysics and cosmology. This edition of NPA-X will highlight novel opportunities in precision nucleosynthesis, neutron star physics, cosmic ray physics and chemical stellar evolution that arise from combining the latest observations...
Go to contribution page -
Zsolt Podolyak05/09/2022, 10:00Invited
Half of the nuclei heavier than iron were synthetized in the r process. The r-process yield peak at A~195 is linked to the N=126 closed neutron shell. In contrast to lighter mass regions, the r-process waiting point nuclei at N=126 still cannot be studied experimentally, and the yield calculations rely entirely on theoretical nuclear physics properties.
Go to contribution page
The most neutron rich N=126 nuclei for... -
Cristian Massimi (Universita e INFN, Bologna (IT))05/09/2022, 10:30Invited
In this presentation, I shall give an overview of neutron-induced cross section measurements at n_TOF, both past and present. A selection of the principal characteristics of the time-of-flight facility n_TOF at CERN is given together with several examples of measurements of interest to Nuclear Astrophysics.
Finally, I will present some ideas of possible future experiments, including the...
Go to contribution page -
Rene Reifarth (Goethe University Frankfurt (DE))05/09/2022, 11:30Invited
The GSI/FAIR facility close to Darmstadt, Germany offers a large suite of experimental possibilities with radioactive ions. Stable ions between hydrogen and uranium can currently be accelerated with the synchrotron SIS-18. Fragmentation on combination with a powerful fragment separator (FRS) enable the experiments with a wide range of radioactive isotopes. Single pass can be used to...
Go to contribution page -
Iris Dillmann (TRIUMF & University of Victoria)05/09/2022, 12:00Oral
Heavy-ion storage rings connected to radioactive beam facilities offer a unique environment for nuclear physics experiments. However, so far they have been only coupled to in-flight fragmentation facilities, for example the ESR and the CRYRING at GSI Darmstadt/ Germany, the CSR at HIRF in Lanzhou/ China, and the Rare RI Ring at RIKEN Nishina Center in Japan.
Go to contribution page
Neutron capture reactions play a... -
Michael Paul05/09/2022, 12:15Oral
The plasma density, temperature and pressure in laser-induced deuterium-tritium (DT) inertial fusion implosions at the National Ignition Facility (NIF) are comparable to those in the center of stars. Neutrons are produced within a radius of $\approx$50 $\mu$m and a time of $\approx$100 ps, representing a uniquely high neutron density approaching 10$^{22}$ cm$^{-3}$, close to that of the...
Go to contribution page -
Moshe Friedman (The Hebrew University of Jerusalem)05/09/2022, 14:00Invited
Neutron-induced reactions play an important role in several stellar nucleosynthesis scenarios. Experimental determination of their rates are limited by the available neutron flux at the relevant energies, sample size, especially in the case of unstable isotopes, and detection. The Soreq Applied Research Accelerator Facility (SARAF) enabled enhanced opportunities for such measurements by...
Go to contribution page -
Dr Faïrouz Hammache (IJCLab Orsay)05/09/2022, 14:30Oral
F. Hammache$^1$, P. Adsley$^{2,3,*}$, L. Lamia$^{4,5,6}$, D.~S. Harrouz$^1$, N. de Séréville$^{1}$, B. Bastin$^7$, T. Faestermann$^{8}$, C. Fougères$^7$, R. Hertenberger$^{9}$, M. La Cognata$^{5}$, A. Meyer$^{1}$, S. Palmerini$^{10,11}$, R.G. Pizzone$^{5}$, F. de Oliveira$^7$, S. Romano$^{4,5,6}$, A. Tumino$^{12,5}$, H.-F. Wirth$^{9}$
$^1$ Université Paris-Saclay, CNRS/IN2P3, IJCLab,...
Go to contribution page -
Heinrich Wilsenach05/09/2022, 14:45Oral
One of the current limitations of predicting the nuclear astrophysics r-process abundance is the lack of experimental data on neutron-capture cross-sections of radioactive neutron-rich isotopes. These cross-sections are also invaluable for nuclear reactions and nuclear structure in general. Their measurement is currently considered impossible due to the instability of the targets and...
Go to contribution page -
Dr László Csedreki (Institute for Nuclear Research (ATOMKI), P.O. Box 51, HU-4001 Debrecen, Hungary)05/09/2022, 15:00Oral
The $^{13}$C(α,n)$^{16}$O reaction is the prevalent neutron source for the main s-process, taking place in thermally pulsing low mass AGB stars. The direct measurement of this reaction at stellar temperature (~ 90 MK), corresponding to a Gamow window between 140 - 230 keV, has so far not been possible due to the very low cross section at these energies.
Go to contribution page
The LUNA collaboration performed the... -
Dr Moshe Tessler (Soreq Nuclear Research Center, Yavne, Israel 81800)05/09/2022, 15:15Oral
Neutron-induced reactions remain at the forefront of experimental investigations for the understanding of stellar nucleosynthesis and chemical evolution of the Galaxy in the region of medium- and heavy-mass nuclides [1]. We report on measurements of the cross section of neutron capture reactions $^{74,80,82}$Se$(n,\gamma)$ and $^{138,140,142}$Ce$(n,\gamma)$ relevant, respectively, to the weak...
Go to contribution page -
Brian Fields (University of Illinois)05/09/2022, 16:00Invited
We will summarize the status of big-bang nucleosynthesis (BBN), which describes the production of the lightest nuclides during the first three minutes of cosmic time. We will emphasize the transformational influence of cosmic microwave background (CMB) experiments culminating today with Planck, which pin down the cosmic baryon density to exquisite precision. Standard BBN combines this with...
Go to contribution page -
Roland Diehl05/09/2022, 16:30Invited
Diffuse gamma-ray emission from the decay of radioactive 26Al and 60Fe is a messenger about the nucleosynthesis activity in our current-day galaxy. Because this material is attributed to ejections from massive stars and their supernovae, we can learn from the gamma-ray signal about massive stars and their feedback into surrounding interstellar medium. Our method of population synthesis of...
Go to contribution page -
Dr Benjamin Wehmeyer (Konkoly Obs & Univ Hertfordshire)05/09/2022, 17:00Oral
In addition to the insights gained by studying the galactic evolution of chemical elements, short lived radioisotopes contain additional information on astrophysical nucleosynthesis sites.
Go to contribution page
Meteorites can carry information about the nucleosynthetic conditions in the early Solar System using short lived radioisotopes [1][2], while detections of live isotopes of cosmic origin in the deep sea... -
Djamila Sarah HARROUZ (IJCLab France)05/09/2022, 17:15Oral
Globular clusters are key grounds for models of stellar evolution and early stages of the formation of galaxies. Abundance anomalies observed in the globular cluster NGC 2419, such as the enhancement of potassium and depletion of magnesium [1] can be explained in terms of an earlier generation of stars polluting the presently observed stars [2]. However, the nature and the properties of the...
Go to contribution page -
Dr Rosanna Depalo (Department of Physics, University of Milan and INFN, Milan, Italy)06/09/2022, 09:00Invited
The cross sections of nuclear reactions relevant for astrophysics are crucial ingredients to understand the energy generation inside stars and the synthesis of the elements. In stars, nuclear reactions take place at energies well below the Coulomb barrier. As a result, their cross sections are often too small to be measured in laboratories on the Earth’s surface, where the signal would be...
Go to contribution page -
Javier Balibrea Correa (Univ. of Valencia and CSIC (ES))06/09/2022, 09:30Oral
One of the crucial ingredients for the improvement of stellar models in the framework of nucleosynthesis studies is the accurate knowledge of neutron capture cross-sections for the different isotopes involved. This type of measurements can shed light on the discrepancies between observed and predicted isotopic abundances by the stellar models and thus help to constrain the stellar media...
Go to contribution page -
Marco La Cognata (Universita e INFN, Catania (IT))06/09/2022, 09:45Oral
Radiative-capture reactions leading to the formation of 7Be bear a particular interest in the field of nuclear astrophysics.
Go to contribution page
The most important ones are the 3He(α,γ)7Be and the 6Li(p,γ)7Be reactions.
The former is one of the primary sources of uncertainty in the prediction of the 7Be and 8B neutrino fluxes, being the first reaction of the 2nd and 3rd branch of the p−p chain. Despite its... -
Beatriz JURADO APRUZZESE06/09/2022, 10:00Oral
Obtaining reliable cross sections for neutron-induced reactions on unstable nuclei nuclei is crucial to our understanding of the stellar nucleosynthesis of heavy elements. However, the measurement of these cross sections is very complicated as both projectile and target are radioactive. The NECTAR (NuclEar reaCTions At storage Rings) project aims to circumvent these problems by using the...
Go to contribution page -
Rosario Gianluca Pizzone (INFN LNS)06/09/2022, 10:15Oral
Nuclear reactions play a key role in the framework of the Big Bang Nucleosynthesis. A network of 12 principal reactions has been identified as the main path which drives the elemental nucleosynthesis in the first twenty minutes of the history of the Universe. Among them an important role is played by neutron-induced reactions, which, from an experimental point of view, are usually a hard task...
Go to contribution page -
Marco Limongi (INAF - Observatory of Rome)06/09/2022, 11:00Invited
-
Arthur CHOPLIN (Université Libre de Bruxelles)06/09/2022, 11:30Oral
Despite considerable progresses over the past few decades, the origin of trans-iron elements is not yet fully understood. In addition to the slow (s) and rapid (r) neutron capture processes, an intermediate neutron capture process (i-process) is thought to exist at neutron densities intermediate between the s- and r-processes. The existence of this process is supported by the observation of...
Go to contribution page -
Sara Palmerini06/09/2022, 11:45Oral
Recent models for evolved low-mass stars (with M <=3 Mo), undergoing the asymptotic giant branch (AGB) phase assume that magnetic flux-tube buoyancy drives the formation of 13C reservoirs in He-rich layers. We illustrate their crucial properties, showing how the low abundance of 13C generated below the convective envelope hampers the formation of primary 14N and the ensuing synthesis of...
Go to contribution page -
Dr Tejpreet Kaur (Panjab University, India)06/09/2022, 12:00Oral
The short-lived radionuclides (SLRs) have a half-life ≤ 100 Myr. The excess abundance of their daughter nuclides in various meteoritic phases confirms the existence of SLRs in the early solar system (ESS). In this work, we have developed Galactic chemical evolution (GCE) models to understand the stellar sources of SLRs, $^{26}$Al, $^{36}$Cl, $^{41}$Ca, $^{53}$Mn, and $^{60}$Fe in the ESS. ...
Go to contribution page -
Alfredo Estrade (Central Michigan University)06/09/2022, 12:15Oral
Accreting neutron stars offer unique opportunities to study the properties of matter in extreme density environments and nuclear processes involving very unstable isotopes. X-ray burst are one of the rich observables that can be used to test models of accreting neutron stars. The burst are driven by thermonuclear reactions near the surface of the neutron star that proceed through (a,p) and...
Go to contribution page -
Anu Kankainen06/09/2022, 14:00Invited
The Ion Guide Isotope Separator On-Line (IGISOL) facility [1] in the JYFL Accelerator Laboratory at the University of Jyväskylä offers plenty of opportunities for r-process studies. At IGISOL, neutron-rich nuclei relevant for the r process have been typically produced using proton-induced fission on natural uranium target. Recently, multinucleon-transfer (MNT) reactions to produce neutron-rich...
Go to contribution page -
Alvaro Tolosa Delgado (University of Jyvaskyla (FI))06/09/2022, 14:30Oral
How elements are made in the Universe is an open long-standing question. Several processes are invoked to explain the observed elemental abundances in our Solar System [1] and in our galaxy [2].
Go to contribution page
Complex astrophysical simulations are used to study the origin of the heavy elements and quantify the contribution of the r-process to the observed elemental abundances (see e.g. [3]). The r-process... -
Dr Thanassis Psaltis (TU Darmstadt)06/09/2022, 14:45Oral
The lighter heavy elements of the first r-process peak, between strontium and silver, can be synthesized in the moderately neutron rich neutrino–driven ejecta of either core–collapse supernovae or neutron star mergers via the weak r–process [1]. This nucleosynthesis scenario exhibits uncertainties from the absence of experimental data from $(\alpha,xn)$ reactions on neutron–rich nuclei, which...
Go to contribution page -
Xilu Wang06/09/2022, 15:00Oral
The astrophysical sites where 𝑟-process elements are synthesized remain mysterious: it is clear that neutron-star-mergers (kilonovae, KNe) contribute, and some classes of core-collapse supernovae (SNe) are also possible sources of at least the lighter 𝑟-process species. The discovery of 60Fe on the Earth and Moon implies that one or more astrophysical explosions have occurred near the Earth...
Go to contribution page -
Cameron Angus (University of York / TRIUMF)06/09/2022, 15:15Oral
The r-process has been shown to be robust in reproducing the abundance distributions of heavy elements seen in ultra-metal poor stars. In contrast, observations of elements in the range 36 ≤ Z ≤ 47 display overabundances relative to r-process model predictions [1]. A proposed solution to this discrepancy is an additional source of early nucleosynthesis that preferentially produces the lighter...
Go to contribution page -
Brian Metzger06/09/2022, 16:00Invited
The astrophysical origin of the rapid neutron capture (r-process) remains an outstanding mystery in nuclear astrophysics. I will review our evolving understanding of potential r-process sites, particularly those associated with the merger of binary neutron stars and the core collapse of massive rotating stars. I will describe how these diverse channels are directly probed by the thermal...
Go to contribution page -
Dr Umberto Battino (University of Hull)06/09/2022, 16:30Oral
The astrophysical origins of the heaviest stable elements that we observe today in the Solar System are still not fully understood. While thermonuclear supernovae (SNe Ia) are known to have forged about two-thirds of the iron content in the Solar System, recent studies have demonstrated that H-accreting white dwarfs (WDs) in a binary system exploding as SNe Ia could be an efficient p-process...
Go to contribution page -
Moritz Reichert06/09/2022, 16:45Oral
Magnetorotational supernovae (MR-SNe) are promising candidates for the enrichment of heavy elements in the early universe. We analyze the nucleosynthesis of four sophisticated 3D (Obergaulinger & Aloy 2021) and two long evolved 2D neutrino-magnetohyrodynamic models (Aloy & Obergaulinger 2021). We identified three main mechanisms to synthesize heavy elements. Namely, an early and prompt...
Go to contribution page -
Stylianos Nikas06/09/2022, 17:00Oral
Binary neutron star mergers have been expected to synthesize r-process elements and emit radiation powered by the radioactive decay of the freshly produced isotopes, called kilonovae. Although the observation of the kilonova was the first direct evidence of the operation of the r-process nucleosynthesis at the GW170817/AT2017gfo event, no trace of individual elements has been identified except...
Go to contribution page -
Sophie Abrahams (University of York)06/09/2022, 17:15Oral
In massive-star binary systems, upon reaching later stages of stellar evolution one star can expand as a giant and envelope its companion. The enveloped companion, here a neutron star, can begin to accrete matter. The angular momentum of the accreting material will result in the formation of an accretion disk. Accretion onto common-envelope-phase neutron stars can result in material ejected...
Go to contribution page -
Dr Lizeth Morales-Gallegos (INFN)06/09/2022, 18:00Poster
$^{12}$C fusion reactions are among the most important in stellar evolution since they determine the destiny of massive stars. Over the past fifty years, massive efforts have been done to measure these reactions at low energies. However, existing data present several discrepancies between sets and large uncertainties specially at the lowest energies. Factors such as beam/environmental...
Go to contribution page -
David Rapagnani (University of Naples "Federico II")06/09/2022, 18:00Poster
When stars approach the red giant branch, a deep convective envelope develops and the products of the CNO cycle appear at the stellar surface. In particular, the $\rm^{17}O$ is enhanced in RGB and AGB stars. Then, spectroscopic analyses of O isotopic ratios of these stars provide a powerful tool to investigate the efficiency of deep mixing processes, such as those powered by convective...
Go to contribution page -
Tanja Heftrich06/09/2022, 18:00Poster
Heavy elements beyond iron are mainly synthesizing neutron capture reactions. The slow neutron capture process (s-process) is responsible for 50\,\% of the heavy elemental abundances. The corresponding neutron energies in the different astrophysical sites range from a few keV to about hundred keV. By using the activation technique, neutron capture reactions have been studied over the last...
Go to contribution page -
Giuseppe D'Agata (Università degli Studi di Catania - Dipartimento di Fisica e Astronomia "Ettore Majorana" & Laboratori Nazionali del Sud - INFN)06/09/2022, 18:00Poster
The presence of ${\rm ^{26}Al}$ (T$_{1/2}$=1.04 Myr) in the interstellar medium has been strongly debated through the years: its 1.809 MeV $\gamma$-ray line has been appointed as a tracer of the recent nucleosynthesis in our galaxy, and its presence have been found spread along Galactic plane. Observations support the idea that this isotope can been formed through nucleosynthesis in massive...
Go to contribution page -
Sukhendu Saha (Saha Institute of Nuclear Physics, HBNI, India)06/09/2022, 18:00Poster
Facility for Research in Experimental Nuclear Astrophysics (FRENA), an upcoming tandem accelerator facility at Saha Institute of Nuclear Physics, Kolkata, India. This is a low energy (0.2-3 MV) high current facility primarily designed for nuclear astrophysical studies. Most of the astrophysical reactions have very low cross-sections with large error bars[1]. So the background studies in this...
Go to contribution page -
Borbála Cseh06/09/2022, 18:00Poster
The Barium (Ba) star phenomenon is unmissable from the study and understanding of nucleosynthetic processes occuring in asymptotic giant branch (AGB) stars. Ba stars belong to binary systems, where the former AGB polluted the companion, a less evolved star, which became enriched with material produced through the slow neutron capture process (s process). While the AGB has evolved to a white...
Go to contribution page -
Nicolae Sandulescu06/09/2022, 18:00Poster
Binding energies, proton-neutron paring and α-like quartetting in proton-rich nuclei
close to N=Z lineN. Sandulescu
National Institute of Physics annd Nuclear Engineering, 76900 Magurele-Bucharest, Romania
The modelling of nucleosynthesis processes triggered by rapid proton capture requires accurate predictions for the binding energies of...
Go to contribution page -
Ruchi Garg (Facility for Rare Isotope Beams, Michigan State University)06/09/2022, 18:00Poster
Stellar explosions such as novae, supernovae, and X-ray bursts involve thermonuclear reactions on rare isotopes. Interpretation of observations such as the light curves from X-ray bursts, elemental abundances, or $\gamma$-rays from nuclear decay as well as predictions of nucleosynthesis are notably impacted by large uncertainties in the nuclear reaction rates. Many of these reactions either...
Go to contribution page -
Mr Thomas Hensel (TU Dresden)06/09/2022, 18:00Poster
The NeuLAND (New Large-Area Neutron Detector) plastic scintillator based time of flight detector for 0.2-1.6 GeV neutrons is currently under construction at the Facility for Antiproton and Ion Research (FAIR), Darmstadt, Germany. In its final configuration, NeuLAND will consist of 3,000 2.7 m long plastic scintillator bars that are read out on each end by fast timing photomultipliers. Here,...
Go to contribution page -
Noshad Khosravi Largani06/09/2022, 18:00Poster
The subject of massive star explosions driven by a first-order hadron-quark matter phase transition has gained increasing attention in the community, e.g., providing a novel path to the existence of massive pulsars of 2 solar masses at birth [1] and the creation of ejected r-process material in these explosive events [2]. However, no final conclusions can yet be drawn from these results about...
Go to contribution page -
Mr Lukas Bott (Goethe University Frankfurt (DE))06/09/2022, 18:00Poster
Over the last decades huge efforts were made to determine the $^{12}$C($\alpha,\gamma$)$^{16}$O cross section, as it is key to understand the evolution of stars. Using direct methods with stable targets and a low-energy ion beam poses significant challenges to the experimental setup and data analysis. Center-of-mass energies down to 1 MeV were reached with sometimes large uncertainties of up...
Go to contribution page -
Anup Yadav (Helmholz-Zentrum Dresden-Rossendorf, Institute of Radiation Physics, Dresden, Germany)06/09/2022, 18:00Poster
For direct cross section measurements in nuclear astrophysics, in addition to suitable ion beams and detectors, also highly pure and stable targets are needed. Here, using a gas jet as a target offer an attractive approach that combines high stability even under significant beam load with excellent purity. Such a target is currently under construction at the Felsenkeller underground ion...
Go to contribution page -
Teodora Andreea Madgearu (Extreme Light Infrastructure - Nuclear Physics/IFIN-HH, Magurele, Romania)06/09/2022, 18:00Poster
The $^{19}$F(p,$\alpha$)$^{16}$O reaction is important for understanding the fluorine abundance in the outer layers of asymptotic giant branch (AGB) stars and it might also play a role in hydrogen-deficient post-AGB star nucleosynthesis. Up to now, theoretical models overproduce F abundances in AGB stars with respect to the observed values, thus calling for further investigation of the...
Go to contribution page -
Philipp Erbacher06/09/2022, 18:00Poster
The neutron activation technique is a well established method to measure neutron capture cross sections relevant for the s-process.The $^{7}$Li(p,n) reaction at E$_{p} = 1912\,$keV is often used as a neutron source since the energy distribution of the emitted neutrons closely resembles a Maxwell-Boltzmann spectrum of $k_{B}T = 25\,$keV mimicking the $^{22}$Ne($\alpha$,n) phase in TP-AGB...
Go to contribution page -
Frederic Lassiaille06/09/2022, 18:00Poster
Null four-vectors of General Relativity (GR), suggest mathematical developments. Two of them are presented. It is reminded that in GR a privileged frame exists, which is the frame in whch time elapses the most. It is showned that a particle generates locally a space-time deformation, which transforms this privileged frame according to the boost associated with its velocity in this frame. From...
Go to contribution page -
Bhusan Kayastha06/09/2022, 18:00Poster
We present some results from the DRAGON simulations, a set of four direct N-body simulations of globular clusters (GCs) with a million stars and five percent initial (primordial) binaries. These simulations were undertaken with the NBODY6++GPU code, which allowed us to follow dynamical and stellar evolution of individual stars and binaries, formation and evolution of white dwarfs, neutron...
Go to contribution page -
Louis-Alexandre Lalanne (KU Leuven (BE))06/09/2022, 18:00Poster
A recent sensitivity study has shown that the 35K(p,γ)36Ca reaction is one of the ten (p,γ) reaction rates that could significantly impact the shape of the calculated X-ray burst light curve [1]. Its reaction rate used up to now in type I X-ray burst calculations was estimated using an old measurement for the mass of 36Ca and theoretical predictions for the partial decay widths of the first 2+...
Go to contribution page -
Zsolt Mátyus06/09/2022, 18:00Poster
Heavier p isotopes are believed to be produced through the $\gamma$-process. The path of $\gamma$-process can be modelled with network calculations. These calculations include about 20000 reactions on more than 2000, mostly unstable nuclei. Theoretical cross section of reactions involving alpha-particles are found to be very sensitive to the alpha-nucleus optical potential, which is not known...
Go to contribution page -
Mihai Mocanu (University of York, UK)06/09/2022, 18:00Poster
Recent measurement of coherent π0 photoproduction on Pb lead to a most accurate determination of the neutron skin, constraining nuclear matter Equation of State (EoS) at around ρ~1ρ0. A natural next step is elucidating the nuclear EoS at higher densities to tune our understanding of the most violent process in the Universe - neutron stars mergers. It was demonstrated that at densities above...
Go to contribution page -
Itoshi Nishimura (Kindai University)06/09/2022, 18:00Poster
The nuclear fission of very neuron-rich nuclei is essential for the termination of the r-process flow on the nuclear chart and the determination of the final abundances. Nevertheless, most of the available fission data for neutron-rich nuclei are based on theory predictions mostly by phenomenological treatments. In this study, we calculated a series of nuclear fission distribution for...
Go to contribution page -
Eugenia Naselli06/09/2022, 18:00Poster
In the frame of the PANDORA (Plasmas for Astrophysics Nuclear Decays Observation and Radiation for Archaeometry) project [1], a new experimental approach aims at measuring, for the first time, in-plasma $\beta$-decays lifetimes as a function of thermodynamical conditions of a plasma-environment able to mimic some stellar-like conditions. Theoretical predictions [2] and former experiments on...
Go to contribution page -
Francesco Pogliano (University of Oslo)06/09/2022, 18:00Poster
Nuclei in the $^{135}$I region have been identified as a possible bottleneck for the i process. Nuclear properties such as the Maxwellian-averaged cross section are indispensable tools when trying to explain nucleosynthetic processes, but the instability of the region prevents us from carrying out direct measurements. In order to investigate it, we propose an indirect approach.
At the Oslo...
Go to contribution page -
Martin Müller (University of Cologne)06/09/2022, 18:00Poster
In spite of decades of research, many observed nuclear abundances remain that can not be reproduced by p-process nucleosynthesis calculations [1].
Go to contribution page
This is mainly due to the lack of constraints for the involved nuclear physics models.
Previous studies have shown that key reactions affecting the abundance of the p-nucleus $^{168}$Yb are the $^{164,166}$Yb($\alpha, \gamma$) reactions and that... -
Benjamin Brueckner (Goethe University Frankfurt)06/09/2022, 18:00Poster
The neutron activation method is well-suited to investigate neutron-capture
Go to contribution page
cross sections relevant for the main s-process component. Neutrons can be pro-
duced via the $^7$Li(p,n) reaction with proton energies of 1912 keV at e.g. Van de
Graaf accelerators, which results in a Maxwellian spectrum of neutrons corre-
sponding to a temperature of k$_\text{B}$T = 25 keV. This mimicks the... -
Simon Rümmler (Helmholz-Zentrum Dresden-Rossendorf, Institute of Radiation Physics, Dresden, Germany)06/09/2022, 18:00Poster
The 3He(α,γ)7Be reaction plays a role in two distinct astrophysical scenarios, solar fusion processes as well as the Big Bang nucleosynthesis. The astrophysical S-factor of this reaction has been studied several times for energies above 0.3MeV and once for energies between 0.1MeV and 0.2MeV, but never directly for energies below 0.1MeV. The energies in between and below the measured range are...
Go to contribution page -
Axel Boeltzig (Helmholtz-Zentrum Dresden-Rossendorf (HZDR))06/09/2022, 18:00Poster
Cross section measurements of ${}^{12,13}\mathrm{C}(\mathrm{p},\gamma){}^{13,14}\mathrm{N}$ have been performed at the Laboratory for Underground Nuclear Astrophysics (LUNA), where the low-background environment and high beam currents of the $400\,\mathrm{kV}$ accelerator allowed to obtain cross section data for these reactions at lower energies and with smaller statistical uncertainties than...
Go to contribution page -
Dr Elizabeth Musacchio Gonzalez (LNL-INFN, Italy), Dr Pierfrancesco Mastinu (LNL-INFN, Italy)06/09/2022, 18:00Poster
To calculate the reaction rate in the neutron capture processes it is common to work with the Maxwellian Average Cross Section (MACS), defined as the reaction rate scaled by the most probable neutron velocity of the Maxwell-Boltzmann distribution. For the s-process mainly, the MACS directly describes the reaction rate inside the stars, for a given temperature and neutron density. Hence, the...
Go to contribution page -
Claudio Santonastaso06/09/2022, 18:00Poster
$^{12}C(\alpha,\gamma)^{16}O$ has been, and still is, one of the central topic in nuclear astrophysics.\
Go to contribution page
Reason for this is that stellar models are very sensitive to the ratio $^{12}C/^{16}O$ produced by the helium buring stage. Knowing the value of the $^{12}C(\alpha,\gamma)^{16}O$ S-factor at the energy of astrophysical interest ($E_0\sim$ 300 keV) to a precision better than 10\% would... -
Dr Alexandra Zadvornaya (Department of Physics, University of Jyväskylä, P.O. Box 35, FI-40014, Finland)06/09/2022, 18:00Poster
Multinucleon-transfer (MNT) reactions have gained a lot of attention in the last decade following the theoretical prediction of larger than expected production cross sections for heavy neutron-rich nuclei [1] playing a key role in the astrophysical rapid neutron capture process (r process) [2]. At the Ion Guide Isotope Separator On-Line (IGISOL) facility [3] in the JYFL Accelerator Laboratory,...
Go to contribution page -
Dr Rugard Dressler (Paul Scherrer Institute (CH))06/09/2022, 18:00Poster
Short-lived radionuclides, i.e. radioactive isotopes with half-lives of less than 100 Ma, were present as primordial isotopes in the proto-solar cloud and during the formation of our solar system. The origin of specific short-lived radionuclides is still a matter of dispute. Because of their comparatively short half-lives, these isotopes are no longer present in cosmic samples today, but are...
Go to contribution page -
David Barba González (University of Salamanca)06/09/2022, 18:00Poster
We perform microscopic Molecular Dynamics simulations to study crystallization in the outer crust of Neutron Stars (NSs). We study the energetics and pressure in the electron screened nuclear system using a consistent nuclear population in the inner and outer crust under the approximation of one the component plasma (OCP) and multicomponent plasma (MCP) assuming some nuclear species...
Go to contribution page -
Dr Chandrabhan Yadav (Racah Institute of Physics, The Hebrew University of Jerusalem, Israel)06/09/2022, 18:00Poster
Neutron-induced charged particle reactions (n, p) and (n, α), especially on unstable proton-rich isotopes, play an important role in understanding explosive astrophysical scenarios and interpreting their remnants. In a recent publication [1], a novel approach is described to study experimental cross-sections of (n, p) and (n, α) reactions at explosive stellar temperatures for various nuclei...
Go to contribution page -
Dr Tamás Szücs (Institute for Nuclear Research (Atomki))06/09/2022, 18:00Poster
The $^3$He($\alpha$,$\gamma$)$^7$Be nuclear reaction has been investigated in several times before [1]. The importance of this reaction is manifested in two astrophysical scenarios. It plays a role in the nucleosynthesis of the Big Bang (BBN) through the production of lithium and is also a branching reaction in the solar p-p chain. The astrophysically relevant energy range of this reaction in...
Go to contribution page -
Dr Laetitia Canete06/09/2022, 18:00Poster
The $^{25}$Al(p,γ)$^{26}$Si reaction is of tremendous interest in nuclear astrophysics. The production of the γ-ray emitter $^{26}$Al ground state can be bypassed in classical novae via the production of $^{26}$Si which decays to an isomeric state of $^{26}$Al. In order to more precisely estimate the amount of $^{26}$Al that is of classical novae origin, it’s crucial to determine the rate of...
Go to contribution page -
Jordan Marsh06/09/2022, 18:00Poster
The CRYRING Array for Reaction Measurements (CARME) has been mounted at CRYRING FAIR and offers a novel methodology for nuclear reaction measurements utilising storage rings. CARME can be used to study direct nuclear reactions of astrophysical interest in addition indirect studies of key nuclear properties and atomic physics experiments. The CARME system has recently been fully installed and...
Go to contribution page -
Dr Varinderjit Kaur (GSSDGS Khalsa College, Patiala (Punjab))06/09/2022, 18:00Poster
Black holes have ignited thought-provoking ideas for decades because of their peculiar origin of existence and very nature. Once only thought to be merely a mathematical curiosity, black holes have now become an integral part of Astrophysics and Astronomy that devour copious amounts of matter. Given the advancement from the first speculation to the latest research, an up-to-date review report...
Go to contribution page -
Dr Sangeeta Arora (Department of Applied Sciences, Chandigarh Engineering College, Landran (Punjab) - 140307, India)06/09/2022, 18:00Poster
The impression of mean field and spectator matter has been studied through the collision geometry dependence of reduced flow and elliptical flow in heavy-ion collisions (HICs) at intermediate energies using Isospin-dependent Quantum Molecular Dynamics (IQMD) model for the reaction of $^{50}_{20}$Ca+$^{50}_{20}$Ca and $^{197}_{79}$Au+$^{197}_{79}$Au at incident energy between 50 MeV/nucleon and...
Go to contribution page -
Christopher Griffin06/09/2022, 18:00Poster
Nuclear data such as masses, half-lives, reaction cross-sections and information on decay modes are vital in developing a deeper understanding of nucleosynthetic processes and the origin of the elements. However, these properties are not always constant, and can depend strongly on the atomic charge state experienced in different stellar environments. When nuclei exist as highly charged ions...
Go to contribution page -
Vicente Garcia Tavora (Consejo Superior de Investigaciones Cientificas (CSIC) (ES))06/09/2022, 18:00Poster
Several reactions of light nuclei require a better understanding in Nuclear Astrophysics. The most relevant one is 12C(α,γ)16O. The reason for this is both, the unmitigated importance of the reaction, and the complexity of its cross section at the relevant energies of static helium burning (300 keV) which uncertainty is still undesirably large. As there is no state of natural parity to serve...
Go to contribution page -
Tsung-Han Yeh (University of Illinois Urbana-Champaign)06/09/2022, 18:00Poster
Big Bang Nucleosynthesis (BBN) accounts for the cosmic origin of the lightest elements, and deuterium (D/H) plays a key role in probing the physics of the early universe. The simplicity of BBN theory allows for few-percent-level precision of D/H prediction, which is not normally possible in nuclear astrophysics. Under such precision, the comparison between predicted and observed primordial D/H...
Go to contribution page -
Dr Daniel Pęcak (Warsaw University of Technology)06/09/2022, 18:00Poster
Bardeen–Cooper–Schrieffer theory explains how the heat capacity of the superfluid vanishes when the temperature approaches zero. Various mechanisms may suppress the pairing gap in the superfluid, leading to an increased heat capacity. In turn, this may translate to changing the cooling rate and the thermal evolution of neutron stars. The presence of a vortex in a superfluid neutron matter will...
Go to contribution page -
Ms Svenja Wilden (University of Cologne)06/09/2022, 18:00Poster
The existence of most of the stable very neutron deficient nuclei - the $p$ nuclei - cannot be explained via neutron-capture reactions. Therefore, at least one other process has to exist in order to describe their origin, the $\gamma$ process. Since most photodisintegration reactions involved in the process are not directly accessible, reliable statistical model calculations are needed to...
Go to contribution page -
Giovanni Luca Guardo06/09/2022, 18:00Poster
The $^{17}$O(n,$\alpha$)$^{14}$C reaction is considered in astrophysical codes for its role in the astrophysically relevant "s(slow)-process" since it could act as a possible “neutron-poison” for the neutron induced nucleosynthesis thus influencing the final stellar abundances of some elements such as Fe, Ni or Sr. Thus, its reaction rate must be known in the energy region of interest for...
Go to contribution page -
Srijan Prasad Rauniyar (Arniko Sceondary School)06/09/2022, 18:00Poster
Muon are the subatomic particles. with very high speed(2.9*10^8).with this speed it can travel a distance of 456meters.But the muon formed in the atmosphere travel the distance of 15 km whish is shown by research.
Go to contribution page
This phenomenon is called muon paradox if we can differentiate between these special muon (of muon paradox which undergoes in time dilation and length contraction) and normal muon... -
Chris Nagele (University of Tokyo)06/09/2022, 18:00Poster
Observed supermassive black holes in the early universe have several proposed formation channels, in part because most of these channels are difficult to probe. One of the more promising channels, the directly collapse of a supermassive star, has several possible probes including the explosion of a helium supermassive star triggered by a general relativistic instability. We develop a...
Go to contribution page -
Magdalena Skurzok06/09/2022, 18:00Poster
The experimental investigation of the low-energy negatively charged kaons interaction with the nuclear matter is very important to understand the strength of the K-nuclei interaction and to provide essential input for understanding of the non-perturbative QCD in the strangeness sector. It has strong consequences in various sectors of physics, like nuclear and particle physics as well as ...
Go to contribution page -
Lalit Kumar Sahoo (SAHA INSTITUTE OF NUCLEAR PHYSICS, HBNI,INDIA)06/09/2022, 18:00Poster
$^{19}$F (p,$\alpha$) reaction is one of the crucial reactions in the CNO Cycle. It has the utmost importance in the astrophysical region particularly below the Coulomb barrier [1]. In an astrophysical scenario, the importance astrophysical S-factor is crucial for the understanding of discrepancies in fluorine nucleosynthesis [2-4] and the contribution of direct or resonance at such low...
Go to contribution page -
Max Pallas I Solis (Universitat Politècnica de Catalunya (UPC))06/09/2022, 18:00Poster
Around half of the elemental abundances heavier than iron are created via the rapid neutron capture process (r-process). For nuclear masses $A>100$, there are two main peaks in the r-process abundances, located at $A\sim 130$ and $A\sim 195$. These peaks are associated with neutron shell closures. In contrast, the rare-earth peak (REP) is a small - but clear - peak around mass $A=160$,...
Go to contribution page -
Frederic Lassiaille06/09/2022, 18:00Poster
The latest developments in Surrounding Matter Theory [1] are presented. They include the fitting to Tully-Fisher law, without regression on the previous model's predictions. A following and ambitious search for of a new type of calculation of General Relativity space-time structure is presented. Some possible insight into Nuclear Physics are mentionned.
Go to contribution page
[1] F. Lassiaille, EPJ Web of Conf ... -
Dr Sriteja Upadhyayula06/09/2022, 18:00Poster
As the slowest reaction in the carbon-nitrogen cycle of hydrogen burning, the $^{14}$N($p,\gamma$)$^{15}$O reaction modulates the rate of energy generation in stars in the cycle and thus determines the time spent on the main sequence. Astrophysical challenges, such as the age determination of globular clusters or the solar-abundance problem can be targeted by improving the precision on the...
Go to contribution page -
Mr Vivek Baruah Thapa (Indian Institute of Technology Jodhpur)06/09/2022, 18:00Poster
The isospin dependent nuclear saturation property has a salient role to play in understanding the matter behaviour at high density regimes. Very recently an improved value of neutron skin thickness of $^{208}\text{Pb}$ was reported in Lead Radius EXperiment-II (PREX-2) to be $R_{\text{skin}}=R_n - R_p=(0.283\pm 0.071)$ fm which corresponds to high estimations of nuclear symmetry energy...
Go to contribution page -
Lorenzo Roberti (Konkoly Observatory, CSFK)06/09/2022, 18:00Poster
The nucleosynthesis of elements heavier than iron in stars is one of the most relevant topics in nuclear astrophysics. The neutron-capture processes made most of the abundances of heavy elements in the solar system, but they are not able to make a number of rare proton-rich stable isotopes (p-nuclei) lying on the left side of the stability valley. The $\gamma$-process, i.e. a chain of...
Go to contribution page -
Alessandro Alberto Oliva (DFA-UniCT, INFN-LNS)06/09/2022, 18:00Poster
Carbon burning is a fundamental process for the advanced stages of a massive star ($ M> 8M_\odot $) evolution. It mainly occurs through the $^{12}C+^{12}C$ fusion, however at temperatures higher than $ 10^9 K $ the $^{12}C+^{16}O $ fusion can become prevalent due to the increased abundance of $ ^ {16} O $ in the ashes of the helium burning. The $ ^{12}C + ^{16} O $ reaction also plays a role...
Go to contribution page -
Dr Diego Vescovi (Goethe University Frankfurt)06/09/2022, 18:00Poster
Present nuclear reaction network computations for astrophysical simulations involve many different types of rates, including neutron-capture reactions of interest for the modeling of heavy-element nucleosynthesis. While for many of them we still have to rely on theoretical calculations, an increasing number of experimentally-determined cross sections have now become available. In this...
Go to contribution page -
Shoya Tanaka (RIKEN Nishina Center for Accelerator-Based Science)06/09/2022, 18:00Poster
Nucleosynthesis by the rapid neutron-capture process (r-process) produces elements heavier than iron via neutron-rich nuclides, observed in the solar system and stars with various metallicities. In the r-process, fission plays a fundamental role by recycling the matter during neutron irradiation and by shaping the final r-abundance distribution. Nevertheless, most of the fission data available...
Go to contribution page -
Cristian Massimi (Universita e INFN, Bologna (IT))06/09/2022, 18:00Poster
We show the impact on AGB stellar nucleosynthesis of the maxwellian averaged capture cross sections determined at n_TOF over the past 20 years. We developed an automated procedure to derive MACSs from evaluated data libraries, which are subsequently used as input to stellar models computed by means of the FUNS code.
Go to contribution page
In this contribution, we present a number of s-process abundances obtained... -
Nobuya Nishimura (RIKEN)06/09/2022, 18:00Poster
The nuclear fission of very neuron-rich nuclei is essential in the r-process for the termination of nucleosynthesis flows and the final abundances. Nevertheless, most of the available fission data for the r-process simulations are based on phenomenological calculations. In the present study, we investigate the theoretical uncertainty of nuclear fission related to the r-process. Focusing on the...
Go to contribution page -
Alexander Holas (Heidelberg Institute for Theoretical Studies)06/09/2022, 18:00Poster
It has long been postulated that the onset of electron captures in degenerate high-density ONe cores of super-AGB stars would trigger a supernova, resulting in a collapse into a neutron star (NS). New models of these so-called electron capture supernovae (ECSNe) suggest that while the full collapse to a NS is still a possibility, the energy release by the electron-capture reactions can also...
Go to contribution page -
Dr Maria Letizia Sergi (UniCT & INFN-LNS)06/09/2022, 18:00Withdrawn
Neutron-induced reactions play an important role in nuclear astrophysics in several scenario, such as Big Bang nucleosynthesis or heavy-element production via the s or r neutron capture processes [1]. To overcome some of the experimental difficulties typical of direct neutron cross section measurements, in the last years, the possibility of using the Trojan Horse Method (THM) to study...
Go to contribution page -
Federico Rizzuti06/09/2022, 18:00Poster
Our knowledge of massive star evolution and nucleosynthesis is limited by uncertainties related to multi-dimensional processes taking place in stellar interiors. Only recently, theoretical works are starting to improve 1D stellar evolution codes with the help of 3D hydrodynamics models, which are used to study multi-D processes on a short time range (minutes or hours) and improve 1D...
Go to contribution page -
Denise Piatti06/09/2022, 18:00Poster
The $^{6}$Li(p, $\gamma$)$^{7}$Be reaction is involved both in Big Bang Nucleosynthesis and $^{6}$Li depletion in pre-main and in main sequence stars.
Go to contribution page
The $^{6}$Li(p, $\gamma$)$^{7}$Be S-factor trend was poorly constrained at astrophysical energies because of conflicting experimental results reported in literature. A recent direct measurement, indeed, found a resonance-like structure at... -
Gianpiero Renato Gervino (Universita e INFN Torino (IT))06/09/2022, 18:00Poster
Two significant anomalies have been recently observed in the emission of electron-positron
Go to contribution page
pairs in the 7Li(p,e− e+)8Be and 3H(p,e− e+)4He reactions [1, 2]. These anomalies have
been interpreted as the signature of the existence of a boson (hereafter referred to as X17)
of mass M_X17 = 16.8 MeV that could be a mediator of a fifth force, characterised by a
strong coupling suppression of... -
Enrique Nacher (Univ. of Valencia and CSIC (ES))07/09/2022, 09:00Invited
Nucleosynthesis in Type I X-ray bursts (XRB) proceeds eventually through the rp-process near the proton drip-line. Several N=Z nuclei act as waiting points in the reaction network chain. Astrophysical calculations of XRB light curves depend upon the theoretical modelling of the beta decays of interest, with the N=Z and their second-neighbours N=Z+2 being key nuclei in this context.
Several...
Go to contribution page -
Rahul Jain (Michigan State University)07/09/2022, 09:30
Low Mass X-ray Binaries that transiently accrete matter onto their neutron stars are excellent laboratories for studying dense matter physics. These systems go in and out of the quiescence phase over observational timescales of decades. Monitoring the surface temperatures of neutron stars in this phase reveals a great deal of information about their structure and composition. However, to infer...
Go to contribution page -
Daniel Bemmerer07/09/2022, 09:45
For low-background cross-section measurements, it is beneficial to host an ion accelerator in an underground setting, shielded from cosmic rays. The Felsenkeller 5 MV underground ion accelerator in Dresden, Germany, is the second such facility in Europe and has recently become accessible using EU-supported transnational access. The contribution will review recent progress at Felsenkeller: The...
Go to contribution page -
Mansi Saxena07/09/2022, 10:00
Type-I X-rays bursts are thermonuclear flashes ignited on the surface of a neutron star which is accreting hydrogen and helium-rich material from its companion star. With an hours-long stellar half-life and a low proton capture Q value (~690 keV), doubly magic 56Ni has long been defined as one of the waiting points in the rapid proton capture (rp) process that powers the type-I X-ray bursts....
Go to contribution page -
Dr Matthew Williams (TRIUMF)07/09/2022, 10:15
Approximately 30 stable nuclides on the neutron-deficient side of stability cannot be produced via the same neutron-capture driven mechanisms responsible for synthesizing all other elements heavier than iron. These “p-nuclei” are instead thought to originate from photodisintegration reactions on s- and r-process seed nuclei, which can occur in the extreme high-temperature environments of...
Go to contribution page -
Gabriel Martínez Pinedo (GSI Darmstadt)07/09/2022, 11:00Invited
A kilonova is an electromagnetic transient powered by the radioactive decay of nuclei freshly
Go to contribution page
synthesized by the rapid neutron capture process (r-process). Its observation following the
gravitational wave event GW170817 provided the first evidence that the r-process operates in
neutron star mergers. Kilonova observations provide unique opportunities to learn about the in-
situ operation of... -
Mr Yukiya Saito07/09/2022, 11:30
The rapid neutron capture process ($r$-process) is a complex nucleosynthesis mechanism for the creation of heavy nuclei, which occurs under extreme astrophysical conditions, such as binary neutron star mergers and core-collapse supernovae. Not only are the predictions of the r-process abundance pattern affected by such astrophysical conditions, the calculations also involve thousands of...
Go to contribution page -
Ms Maria Markova (University of Oslo)07/09/2022, 11:45
The concepts of the nuclear level density (NLD) and $\gamma-$ray strength function (GSF) are two essential tools for the statistical description of excited nuclei and their $\gamma-$decay, used in numerous large-scale astrophysical calculations of abundances of elements in the universe. In this work, one of the widely used experimental techniques, the Oslo method was applied to the...
Go to contribution page -
Felix Heim07/09/2022, 12:00
While most of the heavy elements in our universe are produced via neutron-capture processes, the nucleosynthesis of the neutron-deficient p nuclei is still an open question in nuclear astrophysics. The p nuclei are most likely produced in explosive stellar scenarios by the astrophysical $\gamma$ process, which is a complex network of thousands of nuclear - mostly photodisintegration -...
Go to contribution page -
Dennis Muecher (University of Guelph (CA)), Fabio Zeiser07/09/2022, 12:15
Experimental neutron capture rates of short-lived neutron-rich nuclei are of pivotal importance for our understanding of explosive nucleosynthesis. In this contribution we present an improved method for constraining neutron capture rates in exotic nuclei experimentally with beam intensities down to a few pps using the $\beta$-Oslo method.
While a powerful technique to access the most exotic...
Go to contribution page -
Carlo Bruno (The University of Edinburgh)07/09/2022, 14:00Invited
Storage rings offer a unique approach to measure nuclear reactions using stored radioisotope beams impinging on ultra-pure internal targets. This approach has been pioneered at the ESR storage ring in GSI Laboratory (Germany).
The newly commissioned CRYRING, part of FAIR Phase-0, opens up new and ground-breaking possibilities for nuclear astrophysics at storage rings. CRYRING is the first...
Go to contribution page -
Elisso Stamati (University of Ioannina (GR))07/09/2022, 14:30
Half the atomic nuclei heavier than iron are created through the s-process, i.e. a series of neutron captures and subsequent beta decays. Accordingly, the accuracy of neutron capture rates is of significant importance for these astrophysical calculations and for our understanding of the observed isotopic abundances [1]. In particular, fundamental input can be provided through the determination...
Go to contribution page -
Mr Carlos Paradela Dobarro (European Commission - Joint Resesrch Centre)07/09/2022, 14:45
JRC Geel operates a neutron time-of-flight facility, based on an electron accelerator. At 11 flight paths experiments can be performed simultaneously, with available flight paths ranging from 5m to 400 m. Experimental setups to determine total and reaction cross sections ( capture, elastic and inelastic shattering, fission and charged particle reactions ) are available. Furthermore, during ...
Go to contribution page -
Denise Piatti07/09/2022, 15:00
The $^{17}O(p,\gamma)^{18}F$ reaction plays a crucial role in the hydrogen burning phases of different stellar scenarios. For example, at temperature of interest for AGB nucleosynthesis (20 MK< T < 80 MK) the main contribution to the astrophysical reaction rate come from the poorly constrained ER = 65 keV resonance. The strength of this resonance is presently determined only through indirect...
Go to contribution page -
Ms Shahina (University of Notre Dame)07/09/2022, 15:15
The $^{22}\rm{Ne}(\alpha,\gamma)^{26}\rm{Mg}$ is an important reaction in stellar helium burning environments as it competes directly with one of the main neutron source for the s-process $^{22}\rm{Ne}(\alpha,n)^{25}\rm{Mg}$ reaction. The reaction rate of the $^{22}\rm{Ne}(\alpha,\gamma)^{26}\rm{Mg}$ reaction is dominated by low energy energy resonances at $E_{R}^{lab}$ = 0.65, 0.83 MeV. The...
Go to contribution page -
James deBoer (University of Notre Dame)07/09/2022, 15:30
$(\alpha,n)$ reactions provide a source for neutrons in many stellar environments, fueling the production of the heavy elements. The key $(\alpha,n)$ reactions for the $s$-process are thought to be $^{13}$C and $^{22}$Ne, but reactions on other nuclei, including $^{17,18}$O and $^{24,25}$Mg may also play important roles. In addition, $(\alpha,n)$ reactions are sources of background for...
Go to contribution page -
Artemis Spyrou07/09/2022, 15:45
In recent years the plethora of new astronomical observations has shown that the synthesis of heavy elements cannot be explained just by the three traditional processes (s, r, and p). For this reason, new processes have been proposed that are able to explain these new observations. The ``intermediate'' or i process is one such process and corresponds to neutron densities and time scales...
Go to contribution page -
NPA-X Secretariat07/09/2022, 19:00
VEVEY
Belle Epoque - Diesel-electric paddle boatFreshly renovated! The first paddle boat with diesel-electric propulsion was fully and superbly renovated in 2013. Just as its twin ITALIE, it offers all year round, therefore even in winter, Belle Epoque cruises on Lake Geneva. These two boats are CGN’s only pair of identical Belle Epoque boats to survive after the demolition of the GENERAL...
Go to contribution page -
Shunji Nishimura08/09/2022, 09:00Invited
About half of the elements heavier than iron that exists in nature are believed to be synthesized by astrophysical rapid neutron capture process (r-process), a sequence of neutron captures and $\beta$ decays in extreme neutron-rich stellar environments. The astronomical site and the mechanism of the r-process are not yet fully understood. Reliable nuclear data inputs such as nuclear masses,...
Go to contribution page -
Chloe Fougeres (GANIL (FRANCE))08/09/2022, 09:30Oral
Simulations of explosive nucleosynthesis in novae predict the production of the radioisotope $^{22}\text{Na}$. Its half-life of 2.6 yr makes it a very interesting astronomical observable by allowing space and time correlations with the astrophysical object. This radioisotope should bring constraints on nova models. It may also help to explain abnormal $^{22}\text{Ne}$ abundance observed in...
Go to contribution page -
Francesca Cavanna08/09/2022, 09:45Oral
Light elements were produced in the first few minutes of the Universe through a sequence of nuclear reactions known as Big Bang Nucleosynthesis (BBN). Among the light elements produced during BBN, deuterium is an excellent indicator of cosmological parameters because its abundance is highly sensitive to the primordial baryon density. Although astronomical observations of primordial deuterium...
Go to contribution page -
Dr Laetitia Canete (University of Surrey)08/09/2022, 10:00Oral
We report on a precise mass measurement of 69Co and 70Co performed at the IGISOL facility [1].
Go to contribution page
The nuclear structure above the N=40 subshell closure remained for long unclear due to lack of information on neutron-rich nuclei in this region. This region is known for shape coexistence and intruder states have been observed in neutron-rich cobalt isotopes toward N=40 [2]. The two-neutron... -
Sonja Orrigo (Univ. of Valencia and CSIC (ES))08/09/2022, 10:15Oral
Beta decay has a direct access to the absolute values of the Fermi and Gamow-Teller transition strengths. The comparison with complementary charge exchange reactions, such as the ($^3$He,t) reaction performed on the mirror stable targets at RCNP Osaka, allows us the investigation of fundamental questions related to the role of the isospin in atomic nuclei. A systematic study of...
Go to contribution page -
Jorge Lerendegui Marco (Univ. of Valencia and CSIC (ES))08/09/2022, 11:00Invited
Neutron capture cross-section measurements are fundamental in the study of astrophysical phenomena, such as the slow neutron capture (s-) process of nucleosynthesis operating in red-giant and massive stars. One of the best suited methods to measure neutron capture (n,γ) cross sections over the full stellar range of interest is the time-of-flight (TOF) technique.
TOF neutron capture...
Go to contribution page -
Simone Amaducci (Laboratori Nazionali del Sud (IT))08/09/2022, 11:30Oral
Among the nucleosynthesis mechanism involving the heavy nuclei, the so-called slow (s-)process is one of the better known. Being responsible of about half of the element heavier than iron, many models were built in order to describe the process and the final element abundances.
Go to contribution page
The s-process take place in the inner layers of AGB stars, where the heavy elements are produced during interpulses... -
Sandra Zavatarelli08/09/2022, 11:45Oral
The NeNa and MgAl cycles are relevant to the synthesis of Ne, Na, and Mg isotopes: a detailed knowledge of the involved nuclear processes is fundamental to determine the nucleosynthesis during various stages of stellar evolution, in particular in the Red Giant Branch (RGB) and Asymptotic Giant Branch (AGB) phases, as well as in Novae explosions. Key reactions of these cycles are also thought...
Go to contribution page -
Domenico Santonocito08/09/2022, 12:00Oral
Theory [1,2] predicts that lifetimes of beta-radionuclides can change dramatically as a function of their ionization state. Fully stripped ions in storage rings [3] have proven to change their lifetimes by several orders of magnitudes. The PANDORA (Plasmas for Astrophysics, Nuclear Decay Observation and Radiation for Archaeometry) [4,5] experiment is conceived to measure, for the first time,...
Go to contribution page -
Ragandeep Singh Sidhu (School of Physics and Astronomy, University of Edinburgh, EH9 3FD, UK)08/09/2022, 12:15Oral
Understanding the production and survival of $\mathrm{^{205}{Pb}}$ in stars is pivotal as $\mathrm{^{205}{Pb}}$ is the only short-lived radionuclide that is produced exclusively by the slow neutron capture process (s-process). The ratio of radioactive $\mathrm{^{205}{Pb}}$ to stable $\mathrm{^{204}{Pb}}$, when compared to the expected value from the continuous galactic nucleosynthesis, helps...
Go to contribution page -
Dr Liliana Caballero08/09/2022, 14:00Invited
As standalone detections or in the context of multi-messengers signals, neutrinos offer opportunities to understand our Universe in unprecedented ways. Their weakly interacting nature provides information about the interior of cooling neutron stars, their mergers, and black hole accretion disks. Interpreting neutrino observations from compact objects relies on models of neutrino emission and...
Go to contribution page -
Johann Wiggert Brummer (iThemba LABS)08/09/2022, 14:30Oral
The K600 magnetic spectrometer and the CAKE silicon detector array form a powerful tool for coincidence measurements in many nuclear physics measurements including nuclear astrophysics. These instruments have been used, among others, in studies measuring proton decays from $\alpha$-unbound states in $^{22}$Mg through the $^{24}$Mg(p,t)$^{22}$Mg reaction to study the...
Go to contribution page -
Pelagia Tsintari (Central Michigan University)08/09/2022, 14:45Oral
Neutron-induced reactions are essential to the nucleosynthesis of the elements heavier than iron. Recent studies show that key (n,p) reactions, such as the $^{56}$Ni(n,p)$^{56}$Co and $^{64}$Ge(n,p)$^{64}$Ga, accelerate the so-called neutrino-p process ($\nu$p-process), enabling the process to create heavy elements between nickel (Ni) and tin (Sn) in type II Supernovae. The $\nu$p-process...
Go to contribution page -
Emma Monpribat (Université de Strasbourg, CNRS (FR))08/09/2022, 15:00Oral
Among the reactions driving stellar evolution, $^{12}$C + $^{12}$C fusion gives the key ingredients during carbon burning. This system reveals many resonances [1], but also regions with suppressed fusion cross-sections [2,3]. The reaction was recently measured by the STELLA collaboration utilizing the gamma-particle coincidence technique for precise cross-section measurements reaching down to...
Go to contribution page -
Dr Chiara Mazzocchi (University of Warsaw (PL))08/09/2022, 15:15Oral
Thermonuclear reactions that power the stars take place at different energies according to their respective stellar environments. Such energies are well below the Coulomb barrier and the respective cross-sections are incredibly small, often below experimental reach. Modelling energy production in stars requires experimental data on cross-sections for low energies; these data are sparse. As a...
Go to contribution page -
Moshe Gai (University of Connecticut (US))08/09/2022, 15:30Oral
The carbon/oxygen (C/O) ratio at the end of stellar helium burning is the single most important input to stellar evolution theory. However, it is not known with sufficient accuracy, due to large uncertainties in the cross section of the 12C(a,g)16O reaction. We present results based on a new method, which is significantly different from the experimental efforts of the past four decades [1]....
Go to contribution page -
Diego Vescovi (Goethe University Frankfurt)09/09/2022, 09:00Invited
Asymptotic giant branch (AGB) stars are responsible for the production of the main component, i.e. nuclei from Sr to Pb, of the solar s-process distribution. Despite tremendous advances in the theoretical modeling of these objects over the last few decades, many uncertainties remain. An example is represented by the still-unknown mechanism leading to the $^{13}$C neutron source. The...
Go to contribution page -
Emilio Andrea Maugeri (Paul Scherrer Institute (CH))09/09/2022, 09:30Oral
This contribution highlights the importance of targetry in nuclear physics and astrophysics experiments. Three different stages are described: 1) production, purification and characterization of starting materials, with a concise description of the opportunity offered by PSI in this respect; 2) target manufacture, with emphasis on the last developments obtained at PSI; 3) characterization of...
Go to contribution page -
Dr Alberto Stefanini (INFN - LNL)09/09/2022, 09:45Oral
The study of heavy-ion fusion reactions of light systems is essential for the understanding of the astrophysical reaction networks responsible for the energy production and elemental synthesis in stellar environments. At far sub-barrier energies, fusion is influenced by the hindrance phenomenon [1]. Fusion of light heavy-ions is characterised by a positive Q-value and establishing the presence...
Go to contribution page -
Andrew Ratkiewicz (Lawrence Livermore National Laboratory (LLNL))09/09/2022, 10:00Oral
Neutron-induced reactions on unstable nuclei play an important in nuclear astrophysics and for applications of nuclear technology. However, due to the radioactive nature of the nuclei involved, these reactions are extremely difficult or impossible to directly measure. The importance of these reactions has motivated the development of several indirect methods for constraining their properties,...
Go to contribution page -
Tibor Norbert Szegedi09/09/2022, 10:15Oral
Neutron-rich isotopes between Sr and Ag are thought to be synthesized in the neutrino-driven ejecta of core-collapse supernova explosions via the weak r-process [1]. Recent nucleosynthesis simulations demonstrated that (α,xn) reactions play a crucial role in the formation of these isotopes [1-4]. The rates of the (α,n) reactions are provided by the Hauser-Feshbach model. The main uncertainty...
Go to contribution page -
Jenny Feige09/09/2022, 11:00Invited
Within our solar neighbourhood (150-500 light years) tens of star explosions, i.e., supernovae, occurred within the last ~10 Myr. Their expanding shock fronts swept across our Solar System leaving traces of newly formed nucleosynthesis products on Earth, particularly long-lived radioactive nuclei such as $^{60}$Fe (t$_{1/2}$=2.6 Myr). I will present an overview on (1) accelerator mass...
Go to contribution page -
Raffaele Buompane (University of Campania and INFN-Naples)09/09/2022, 11:30Oral
The $\rm ^7Be(p,\gamma)^8B$ represents one of the more important reaction for the prediction of high energy component of solar neutrino spectrum. The importance of this reaction triggered an intense experimental work over the last decades, where discrepancies were observed between the results of different measurements.
Go to contribution page
The origin of this discrepancy limit the overall precision and accuracy of... -
Nadine Mariel Chiera09/09/2022, 11:45Oral
Precise nuclear data is extremely important for several scientific applications, ranging from the calculation of reaction rates for the description of galactic events, to the evaluation of the toxicity of nuclear waste. As it was recently shown, the re-evaluated half-life data of a considerable number of radionuclides (e.g., Fe-60 [1], Se-79 [2, 3], and Sm-146 [4]) was in substantial...
Go to contribution page -
Giuseppe Cardella09/09/2022, 12:00Oral
Recently we measured the gamma decay probability of 12C levels over the threshold for particle decay as the Hoyle and the 9.64 MeV levels [1] measuring for the first time the two gamma decay of such last level. We observe in our data a large gamma decay width, 3 times larger than the already larger than systematic result of Kibedi et al [2]. Investigating also on the 3-alpha decay channel of...
Go to contribution page -
Sophia Florence Dellmann (Goethe University Frankfurt)09/09/2022, 12:15Oral
By combining two unique facilities at GSI (Helmholtz Centre for Heavy Ion Research),
Go to contribution page
the fragment separator (FRS) and the experimental storage ring (ESR), the first direct measurement of a proton capture reaction of a stored radioactive isotope has been accomplished. The combination of sharp ion energy, ultra-thin internal gas target, and the ability to adjust energy of the beam in the ring... -
Alberto Mengoni (ENEA & INFN, Bologna), Sean John Freeman (CERN)09/09/2022, 12:30
-
Alberto Mengoni (ENEA & INFN, Bologna), Sean John Freeman (CERN)Invited
-
Prof. Cristiana Oprea (JINR)Withdrawn
An analysis of the co-occurrence of several nuclear mechanisms responsible for generating Sn p-nuclei for photon and proton energies up to 25 MeV was conducted. The astrophysical temperature during nucleosynthesis lies in the region of 0.01<T9<10 (that nearly corresponds to incident particle energies < 1 MeV). There is one p-nucleus among those considered, 112Sn, that is bypassed by a low...
Go to contribution page -
Sema Kucuksucu (Dr.)Withdrawn
One of the main goals of modern nuclear physics and astrophysics is to determine the neutron induced reaction cross sections in stars and various astrophysical events such as supernova explosions and neutron star mergers. Modeling the cross sections is essential, since in many cases astrophysically important reactions involve nuclei that are beyond the reach of the most advanced experimental...
Go to contribution page
Choose timezone
Your profile timezone: