Pub Date : 2023-03-15DOI: 10.1051/epjconf/202327902003
T. Kaur
The short-lived radionuclides (SLRs) have a half-life ≤ 100 Myr. The γ-ray observations and excess abundance of their daughter nuclides in various meteoritic phases confirm the existence of SLRs in the Galaxy and early solar system (ESS), respectively. In this work, we have developed Galactic Chemical Evolution (GCE) models for SLRs, 26Al, and 60Fe along with 36Cl, 41Ca, and 53Mn. These models predict the temporal and spatial evolution of SLR abundance trends in the Galaxy from 2-18 kpc. The abundance of two SLRs, 26Al, and 60Fe, are investigated further, as their γ-ray observations are available for comparison with the model predictions. The predictions for the abundance per unit area for each ring show the decreases from the inner to outer regions of the Galaxy. The GCE predictions for the total mass of alive 26Al, and 60Fe in 2-18 kpc of the Galaxy at present time are 0.2 M⊙ and 0.08 M⊙, respectively.
{"title":"Short-lived Radionuclides in the Milky Way Galaxy","authors":"T. Kaur","doi":"10.1051/epjconf/202327902003","DOIUrl":"https://doi.org/10.1051/epjconf/202327902003","url":null,"abstract":"The short-lived radionuclides (SLRs) have a half-life ≤ 100 Myr. The γ-ray observations and excess abundance of their daughter nuclides in various meteoritic phases confirm the existence of SLRs in the Galaxy and early solar system (ESS), respectively. In this work, we have developed Galactic Chemical Evolution (GCE) models for SLRs, 26Al, and 60Fe along with 36Cl, 41Ca, and 53Mn. These models predict the temporal and spatial evolution of SLR abundance trends in the Galaxy from 2-18 kpc. The abundance of two SLRs, 26Al, and 60Fe, are investigated further, as their γ-ray observations are available for comparison with the model predictions. The predictions for the abundance per unit area for each ring show the decreases from the inner to outer regions of the Galaxy. The GCE predictions for the total mass of alive 26Al, and 60Fe in 2-18 kpc of the Galaxy at present time are 0.2 M⊙ and 0.08 M⊙, respectively.","PeriodicalId":11731,"journal":{"name":"EPJ Web of Conferences","volume":"187 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-03-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"88946847","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-03-09DOI: 10.1051/epjconf/202328301002
A. Watson
A brief history of the development of surface detectors for the study of the high-energy cosmic rays is presented. The paper is based on an invited talk given at UHECR2022 held in L’Aquila, 3 – 7 October 2022. In a complementary talk, P Sokolsky discussed the development of the fluorescence technique for air-shower detection.
{"title":"A Brief History of the Study of High Energy Cosmic Rays using Arrays of Surface Detectors","authors":"A. Watson","doi":"10.1051/epjconf/202328301002","DOIUrl":"https://doi.org/10.1051/epjconf/202328301002","url":null,"abstract":"A brief history of the development of surface detectors for the study of the high-energy cosmic rays is presented. The paper is based on an invited talk given at UHECR2022 held in L’Aquila, 3 – 7 October 2022. In a complementary talk, P Sokolsky discussed the development of the fluorescence technique for air-shower detection.","PeriodicalId":11731,"journal":{"name":"EPJ Web of Conferences","volume":"1 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-03-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"83042082","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-03-05DOI: 10.1051/epjconf/202328305010
M. Reininghaus, T. Sjostrand, M. Utheim
Hadronic interaction models are a core ingredient of simulations of extensive air showers and pose the major source of uncertainties of predictions of air shower observables. Recently, Pythia 8, a hadronic interaction model popular in accelerator-based high-energy physics, became usable in air shower simulations as well. We have integrated Pythia 8 with its new capabilities into the air shower simulation framework CORSIKA 8. First results show significantly shallower shower development, which we attribute to higher cross-section predictions by the new simplified nuclear model of Pythia.
{"title":"Pythia 8 as hadronic interaction model in air shower simulations","authors":"M. Reininghaus, T. Sjostrand, M. Utheim","doi":"10.1051/epjconf/202328305010","DOIUrl":"https://doi.org/10.1051/epjconf/202328305010","url":null,"abstract":"Hadronic interaction models are a core ingredient of simulations of extensive air showers and pose the major source of uncertainties of predictions of air shower observables. Recently, Pythia 8, a hadronic interaction model popular in accelerator-based high-energy physics, became usable in air shower simulations as well. We have integrated Pythia 8 with its new capabilities into the air shower simulation framework CORSIKA 8. First results show significantly shallower shower development, which we attribute to higher cross-section predictions by the new simplified nuclear model of Pythia.","PeriodicalId":11731,"journal":{"name":"EPJ Web of Conferences","volume":"192 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-03-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"75696235","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-02-24DOI: 10.1051/epjconf/202227401013
G. Mathews, Atul Kedia, H. Kim, I. Suh
As neutron stars merge they can approach very high nuclear density. Here, we summarized recent results for the evolution and gravitational wave emission from binary-neutron star mergers using a a variety of nuclear equations of state with and without a crossover transition to quark matter. We discuss how the late time gravitational wave emission from binary neutron star mergers may possibly reveal the existence of a crossover transition to quark matter.
{"title":"Neutron Star Mergers and the Quark Matter Equation of State","authors":"G. Mathews, Atul Kedia, H. Kim, I. Suh","doi":"10.1051/epjconf/202227401013","DOIUrl":"https://doi.org/10.1051/epjconf/202227401013","url":null,"abstract":"As neutron stars merge they can approach very high nuclear density. Here, we summarized recent results for the evolution and gravitational wave emission from binary-neutron star mergers using a a variety of nuclear equations of state with and without a crossover transition to quark matter. We discuss how the late time gravitational wave emission from binary neutron star mergers may possibly reveal the existence of a crossover transition to quark matter.","PeriodicalId":11731,"journal":{"name":"EPJ Web of Conferences","volume":"274 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-02-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"75134670","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-02-15DOI: 10.1051/epjconf/202327910003
V. Thapa, M. Sinha
Recently an improved value of neutron skin thickness of 208Pb was reported in Lead Radius EXperiment-2 (PREX-2) to be Rskin = Rn Rp = (0.283 0.071) fm which corresponds to high estimations of nuclear symmetry energy (Esym) and its slope (Lsym). The updated values of Esym and Lsym commensurating to the neutron star observable estimations lie exterior to the astrophysical observed range. The higher values of Lsym at n0 deduced from recent PREX-2 data correlates to matter being easily deformable (yielding higher radius values) around intermediate matter densities leading to higher values of Λ̃ creating a tension between the terrestrial and astrophysical observations. In this study, we exploit this tension to constrain the Δ-scalar meson coupling parameter space.
{"title":"Tension between implications from PREX-2 data and gravitational tidal response on dense matter equation of state","authors":"V. Thapa, M. Sinha","doi":"10.1051/epjconf/202327910003","DOIUrl":"https://doi.org/10.1051/epjconf/202327910003","url":null,"abstract":"Recently an improved value of neutron skin thickness of 208Pb was reported in Lead Radius EXperiment-2 (PREX-2) to be Rskin = Rn Rp = (0.283 0.071) fm which corresponds to high estimations of nuclear symmetry energy (Esym) and its slope (Lsym). The updated values of Esym and Lsym commensurating to the neutron star observable estimations lie exterior to the astrophysical observed range. The higher values of Lsym at n0 deduced from recent PREX-2 data correlates to matter being easily deformable (yielding higher radius values) around intermediate matter densities leading to higher values of Λ̃ creating a tension between the terrestrial and astrophysical observations. In this study, we exploit this tension to constrain the Δ-scalar meson coupling parameter space.","PeriodicalId":11731,"journal":{"name":"EPJ Web of Conferences","volume":"147 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-02-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"88095223","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-02-14DOI: 10.1051/epjconf/202328004003
D. Soldin
High-energy cosmic rays interact in the Earth’s atmosphere and produce extensive air showers (EASs) which can be measured with large detector arrays at the ground. The interpretation of these measurements relies on models of the EAS development which represents a challenge as well as an opportunity to test quantum chromodynamics (QCD) under extreme conditions. The EAS development is driven by hadron-ion collisions under low momentum transfer in the non-perturbative regime of QCD. Under these conditions, hadron production cannot be described using first principles and these interactions cannot be probed with existing collider experiments. Thus, accurate measurements of the EAS development provide a unique probe of multi-particle production in hadronic interactions.
{"title":"Probing Hadronic Interactions with Cosmic Rays","authors":"D. Soldin","doi":"10.1051/epjconf/202328004003","DOIUrl":"https://doi.org/10.1051/epjconf/202328004003","url":null,"abstract":"High-energy cosmic rays interact in the Earth’s atmosphere and produce extensive air showers (EASs) which can be measured with large detector arrays at the ground. The interpretation of these measurements relies on models of the EAS development which represents a challenge as well as an opportunity to test quantum chromodynamics (QCD) under extreme conditions. The EAS development is driven by hadron-ion collisions under low momentum transfer in the non-perturbative regime of QCD. Under these conditions, hadron production cannot be described using first principles and these interactions cannot be probed with existing collider experiments. Thus, accurate measurements of the EAS development provide a unique probe of multi-particle production in hadronic interactions.","PeriodicalId":11731,"journal":{"name":"EPJ Web of Conferences","volume":"1 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-02-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"82594361","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-02-14DOI: 10.1051/epjconf/202328304001
N. Globus, R. Blandford
Understanding the acceleration of Ultra High Energy Cosmic Rays is one of the great challenges of contemporary astrophysics. In this short review, we summarize the general observational constraints on their composition, spectrum and isotropy which indicate that nuclei heavier than single protons dominate their spectra above ˜ 5 EeV, that they are strongly suppressed above energies ˜ 50 EeV, and that the only significant departure from isotropy is a dipole. Constraints based upon photopion and photodisintegration losses allow their ranges and luminosity density to be estimated. Three general classes of source model are discussed - magnetospheric models (including neutron stars and black holes), jet models (including Gamma Ray Bursts, Active Galactic Nuclei and Tidal Disruption Events) and Diffusive Shock Acceleration models (involving large accretion shocks around rich clusters of galaxies). The value of constructing larger and more capable arrays to measure individual masses at the highest energies and probably identifying their sources is emphasized.
{"title":"Ultra High Energy Cosmic Ray Source Models: Successes, Challenges and General Predictions","authors":"N. Globus, R. Blandford","doi":"10.1051/epjconf/202328304001","DOIUrl":"https://doi.org/10.1051/epjconf/202328304001","url":null,"abstract":"Understanding the acceleration of Ultra High Energy Cosmic Rays is one of the great challenges of contemporary astrophysics. In this short review, we summarize the general observational constraints on their composition, spectrum and isotropy which indicate that nuclei heavier than single protons dominate their spectra above ˜ 5 EeV, that they are strongly suppressed above energies ˜ 50 EeV, and that the only significant departure from isotropy is a dipole. Constraints based upon photopion and photodisintegration losses allow their ranges and luminosity density to be estimated. Three general classes of source model are discussed - magnetospheric models (including neutron stars and black holes), jet models (including Gamma Ray Bursts, Active Galactic Nuclei and Tidal Disruption Events) and Diffusive Shock Acceleration models (involving large accretion shocks around rich clusters of galaxies). The value of constructing larger and more capable arrays to measure individual masses at the highest energies and probably identifying their sources is emphasized.","PeriodicalId":11731,"journal":{"name":"EPJ Web of Conferences","volume":"2015 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-02-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"86204592","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-02-09DOI: 10.1051/epjconf/202328303002
A. Matteo, L. Anchordoqui, T. Bister, R. D. Almeida, O. Deligny, L. Deval, G. Farrar, U. Giaccari, G. Golup, R. Higuchi, J. Kim, M. Kuznetsov, I. Marics, G. Rubtsov, P. Tinyakov, F. Urban
After over 60 years, the powerful engines that accelerate ultra-high-energy cosmic rays (UHECRs) to the formidable energies at which we observe them from Earth remain mysterious. Assuming standard physics, we expect UHECR sources to lie within the local Universe (up to a few hundred Mpc). The distribution of matter in the local Universe is anisotropic, and we expect this anisotropy to be imprinted on the distribution of UHECR arrival directions. Even though intervening intergalactic and Galactic magnetic fields deflect charged UHECRs and can distort these anisotropies, some amount of information on the distribution of the sources is preserved. In this proceedings contribution, we present the results of the joint Pierre Auger Observatory and Telescope Array searches for (a) the largest-scale anisotropies (the harmonic dipole and quadrupole) and (b) correlations with a sample of nearby starburst galaxies and the 2MRS catalogue tracing stellar mass within 250 Mpc. This analysis updates our previous results with the most recent available data, notably with the addition of 3 years of new Telescope Array data. The main finding is a correlation between the arrival directions of 12.1%−3.1%+4.5% of UHECRs detected with E ≥ 38 EeV by Auger or with E ≳ 49 EeV by TA and the positions of nearby starburst galaxies on a 15.1°−3.0°+4.6° angular scale, with a 4.7σ post-trial significance, up from 4.2σ obtained in our previous study.
{"title":"2022 report from the Auger-TA working group on UHECR arrival directions","authors":"A. Matteo, L. Anchordoqui, T. Bister, R. D. Almeida, O. Deligny, L. Deval, G. Farrar, U. Giaccari, G. Golup, R. Higuchi, J. Kim, M. Kuznetsov, I. Marics, G. Rubtsov, P. Tinyakov, F. Urban","doi":"10.1051/epjconf/202328303002","DOIUrl":"https://doi.org/10.1051/epjconf/202328303002","url":null,"abstract":"After over 60 years, the powerful engines that accelerate ultra-high-energy cosmic rays (UHECRs) to the formidable energies at which we observe them from Earth remain mysterious. Assuming standard physics, we expect UHECR sources to lie within the local Universe (up to a few hundred Mpc). The distribution of matter in the local Universe is anisotropic, and we expect this anisotropy to be imprinted on the distribution of UHECR arrival directions. Even though intervening intergalactic and Galactic magnetic fields deflect charged UHECRs and can distort these anisotropies, some amount of information on the distribution of the sources is preserved. In this proceedings contribution, we present the results of the joint Pierre Auger Observatory and Telescope Array searches for (a) the largest-scale anisotropies (the harmonic dipole and quadrupole) and (b) correlations with a sample of nearby starburst galaxies and the 2MRS catalogue tracing stellar mass within 250 Mpc. This analysis updates our previous results with the most recent available data, notably with the addition of 3 years of new Telescope Array data. The main finding is a correlation between the arrival directions of 12.1%−3.1%+4.5% of UHECRs detected with E ≥ 38 EeV by Auger or with E ≳ 49 EeV by TA and the positions of nearby starburst galaxies on a 15.1°−3.0°+4.6° angular scale, with a 4.7σ post-trial significance, up from 4.2σ obtained in our previous study.","PeriodicalId":11731,"journal":{"name":"EPJ Web of Conferences","volume":"63 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-02-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"84479657","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-02-01DOI: 10.1051/epjconf/202327603004
R. Schotter
In these proceedings, two multi-differential analyses performed in pp collisions collected by the ALICE collaboration during the LHC Run 2 are presented. One investigates the dependence of strange particle production with multiplicity and effective energy, whereas the other clarifies how strangeness enhancement is correlated to the leading jet in the event. The results suggest that strangeness production at the LHC depends strongly on effective energy, and originates dominantly from the transverse region with respect to the leading jet direction.
{"title":"A multi-differential investigation of strangeness production in pp collisions with ALICE","authors":"R. Schotter","doi":"10.1051/epjconf/202327603004","DOIUrl":"https://doi.org/10.1051/epjconf/202327603004","url":null,"abstract":"In these proceedings, two multi-differential analyses performed in pp collisions collected by the ALICE collaboration during the LHC Run 2 are presented. One investigates the dependence of strange particle production with multiplicity and effective energy, whereas the other clarifies how strangeness enhancement is correlated to the leading jet in the event. The results suggest that strangeness production at the LHC depends strongly on effective energy, and originates dominantly from the transverse region with respect to the leading jet direction.","PeriodicalId":11731,"journal":{"name":"EPJ Web of Conferences","volume":"17 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"89590164","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-01-26DOI: 10.1051/epjconf/202327906004
J. Balibrea-Correa, V. Babiano-Suárez, J. Lerendegui-Marco, C. Domingo-Pardo, I. Ladarescu, A. Tarifeño-Saldivia, V. Alcayne, D. Cano-Ott, E. Gonz'alez-Romero, T. Mart'inez, E. Mendoza, J. Plaza, A. S'anchez-Caballero, F. Calviño, A. Casanovas, C. Guerrero, S. Heinitz, U. Koster, E. Maugeri, R. Dressler, D. Schumann, I. Monch, S. Cristallo, C. Lederer-Woods, O. Aberle, S. Altieri, S. Amaducci, J. Andrzejewski, M. Bacak, C. Beltrami, S. Bennett, A. Bernardes, E. Berthoumieux, M. Boromiza, D. Bosnar, M. Caamano, M. Calviani, F. Cerutti, G. Cescutti, S. Chasapoglou, E. Chiaveri, P. Colombetti, N. Colonna, P. C. Camprini, G. Cort'es, M. A. Cort'es-Giraldo, L. Cosentino, S. Dellmann, M. D. Castro, S. Maria, M. Diakaki, M. Dietz, E. Dupont, I. Dur'an, Z. Eleme, S. Fargier, B. Fern'andez, B. Fern'andez-Dom'inguez, P. Finocchiaro, S. Fiore, V. Furman, F. Garc'ia-Infantes, A. Gawlik-Ramikega, G. Gervino, S. Gilardoni, F. Gunsing, C. Gustavino, J. Heyse, W. Hillman, D. Jenkins, E. Jericha, A. Junghans, Y. Kadi, K.
One of the crucial ingredients for the improvement of stellar models is the accurate knowledge of neutron capture cross-sections for the different isotopes involved in the s-,r- and i- processes. These measurements can shed light on existing discrepancies between observed and predicted isotopic abundances and help to constrain the physical conditions where these reactions take place along different stages of stellar evolution. In the particular case of the radioactive 94Nb, the 94Nb(n,γ) cross-section could play a role in the determination of the s-process production of 94Mo in AGB stars, which presently cannot be reproduced by state-of-the-art stellar models. There are no previous 94Nb(n,γ) experimental data for the resolved and unresolved resonance regions mainly due to the difficulties in producing highquality samples and also due to limitations in conventional detection systems commonly used in time-of-flight experiments. Motivated by this situation, a first measurement of the 94Nb(n,γ) reaction was carried out at CERN n_TOF, thereby exploiting the high luminosity of the EAR2 area in combination with a new detection system of small-volume C6D6-detectors and a high quality 94Nb-sample. The latter was based on hyper-pure 93Nb material activated at the high-flux reactor of ILL-Grenoble. An innovative ring-configuration detection system in close geometry around the capture sample allowed us to significantly enhance the signal-to-background ratio. This set-up was supplemented with two conventional C6D6-detectors and a highresolution LaCl3(Ce)-detector, which will be employed for addressing reliably systematic effects and uncertainties. At the current status of the data analysis, 18 resonance in 94Nb+n have been observed for the first time in the neutron energy range from thermal up to 10 keV.
{"title":"First measurement of the 94Nb(n,γ) cross section at the CERN n_TOF facility","authors":"J. Balibrea-Correa, V. Babiano-Suárez, J. Lerendegui-Marco, C. Domingo-Pardo, I. Ladarescu, A. Tarifeño-Saldivia, V. Alcayne, D. Cano-Ott, E. Gonz'alez-Romero, T. Mart'inez, E. Mendoza, J. Plaza, A. S'anchez-Caballero, F. Calviño, A. Casanovas, C. Guerrero, S. Heinitz, U. Koster, E. Maugeri, R. Dressler, D. Schumann, I. Monch, S. Cristallo, C. Lederer-Woods, O. Aberle, S. Altieri, S. Amaducci, J. Andrzejewski, M. Bacak, C. Beltrami, S. Bennett, A. Bernardes, E. Berthoumieux, M. Boromiza, D. Bosnar, M. Caamano, M. Calviani, F. Cerutti, G. Cescutti, S. Chasapoglou, E. Chiaveri, P. Colombetti, N. Colonna, P. C. Camprini, G. Cort'es, M. A. Cort'es-Giraldo, L. Cosentino, S. Dellmann, M. D. Castro, S. Maria, M. Diakaki, M. Dietz, E. Dupont, I. Dur'an, Z. Eleme, S. Fargier, B. Fern'andez, B. Fern'andez-Dom'inguez, P. Finocchiaro, S. Fiore, V. Furman, F. Garc'ia-Infantes, A. Gawlik-Ramikega, G. Gervino, S. Gilardoni, F. Gunsing, C. Gustavino, J. Heyse, W. Hillman, D. Jenkins, E. Jericha, A. Junghans, Y. Kadi, K. ","doi":"10.1051/epjconf/202327906004","DOIUrl":"https://doi.org/10.1051/epjconf/202327906004","url":null,"abstract":"One of the crucial ingredients for the improvement of stellar models is the accurate knowledge of neutron capture cross-sections for the different isotopes involved in the s-,r- and i- processes. These measurements can shed light on existing discrepancies between observed and predicted isotopic abundances and help to constrain the physical conditions where these reactions take place along different stages of stellar evolution.\u0000In the particular case of the radioactive 94Nb, the 94Nb(n,γ) cross-section could play a role in the determination of the s-process production of 94Mo in AGB stars, which presently cannot be reproduced by state-of-the-art stellar models. There are no previous 94Nb(n,γ) experimental data for the resolved and unresolved resonance regions mainly due to the difficulties in producing highquality samples and also due to limitations in conventional detection systems commonly used in time-of-flight experiments.\u0000Motivated by this situation, a first measurement of the 94Nb(n,γ) reaction was carried out at CERN n_TOF, thereby exploiting the high luminosity of the EAR2 area in combination with a new detection system of small-volume C6D6-detectors and a high quality 94Nb-sample. The latter was based on hyper-pure 93Nb material activated at the high-flux reactor of ILL-Grenoble. An innovative ring-configuration detection system in close geometry around the capture sample allowed us to significantly enhance the signal-to-background ratio. This set-up was supplemented with two conventional C6D6-detectors and a highresolution LaCl3(Ce)-detector, which will be employed for addressing reliably systematic effects and uncertainties.\u0000At the current status of the data analysis, 18 resonance in 94Nb+n have been observed for the first time in the neutron energy range from thermal up to 10 keV.","PeriodicalId":11731,"journal":{"name":"EPJ Web of Conferences","volume":"275 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-01-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"73648353","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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