Feng-Lei Liu
Central China Normal University
March. 19th, 2024
References:
Eur.Phys.J.C 82 (2022) 4, 350
Phys.Lett.B 848 (2024) 138355
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Julien Froustey
N3AS at North Carolina State University
March. 5th, 2024
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Abe Flores
Washington University in St. Louis
Feb. 20th, 2024
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Damiano Fiorillo
Niels Bohr Institute
Feb. 6th, 2024
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Joshua Lin
Massachusetts Institute of Technology
Jan. 23rd, 2024
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Saad Nabeebaccus
Paris-Saclay University
Jan. 16th, 2024
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Cristina Benso
Karlsruhe Institute for Technology
Dec. 12th, 2023
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Bigeng Wang
University of Kentucky
Dec. 5th, 2023
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Thimo Preis
Heidelberg University
Nov. 21st, 2023
References: arXiv:2209.14883 and arXiv:2307.07545
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Andres Ruiz
IBM Quantum France
Nov. 7th, 2023
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Axel Gross
University of Minnesota
Oct. 17th, 2023
We present a model for abundances of heavy elements in metal-poor stars. These stars form early in the history of the interstellar medium (ISM), before contributions from Type 1a supernovae and other events associated with low-mass stars become significant, and are therefore dominated by contributions from Type II supernovae and neutron star mergers associated with massive stars. We take a data-driven approach: the abundances can be explained by the contributions of a small number of unknown sources, which will be constrained by the data. We average the contributions of each source type: each source produces a characteristic amount of each element, which mixes with a characteristic region of the ISM to produce a characteristic concentration. We define a template to be the pattern of elemental concentrations produced by a particular source type. The elemental abundances observed in a metal-poor star should therefore be a linear combination of the templates of the different source types, with the mixing coefficients representative of the number of events of a given type. We constrain the possible templates using the 4th data release of the R-Process Alliance, which provides accurate abundances of Fe, Sr, Ba, and Eu for 195 stars. We find that the dataset can be well fit by the combination of two templates: one dominantly producing Fe and Sr, which we identify as Type II supernovae, and the other producing Sr, Ba, and Eu, which we identify as neutron star mergers. With these templates, the data for (140,190,192) out of 195 stars can be fit within (1,2,3) σ. We constrain the relative production of the templates, and find the Sr production of supernova is several times less than that of neutron star mergers. We discuss the implications of these results for production mechanisms in neutron star mergers. This work is the first rigorous analysis of the abundance data to derive production templates of astrophysical sources, and demonstrates for the first time that Type II supernovae are required to produce Sr in addition to neutron star mergers.
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Xincheng Lin
Duke University
Oct. 3rd, 2023
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Francesca Bonaiti
Johannes-Gutenberg University
June 20th, 2023
[1] F. Bonaiti, S. Bacca, G. Hagen, Ab-initio coupled-cluster calculations of ground and dipole excited states in 8He, Phys. Rev. C 105, 034313 (2022).
[2] B. Acharya, S. Bacca, F. Bonaiti et al., Uncertainty quantification in electromagnetic observables of nuclei, Front. In Phys. 10:1066035 (2023).
[3] R. W. Fearick, P. von Neumann-Cosel, S. Bacca, J. Birkhan, F. Bonaiti et al., in preparation.
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Wenyang Qian
University of Santiago de Compostela
June 6th, 2023
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Fernando Romero-Lopez
Massachusetts Institute of Technology
May 16th, 2023
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Eamonn Weitz
SUBATECH, Nantes Université
May 2nd, 2023
[1]: Caron-Huot, arxiv: 0811.1603
[2]: Ghiglieri, Weitz, arxiv: 2207.08842
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Brendan Reed
Indiana University
April 18th, 2023
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Sonali Patnaik
College of Basic Sciences and Humanities (CBSH), OUAT, Bhubaneswar Ind
April 4th, 2023
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Pedro Espino
Network for Neutrinos, Nuclear Astrophysics, and Symmetries
Mar. 21st, 2023
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Kyle Godbey
Facility for Rare Isotope Beams
Mar. 7th, 2023
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Theo Jacobson
University of Minnesota
Feb. 21, 2023
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Wenbin Zhao
Wayne State University
Feb. 7, 2023
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Peter Gysbers
University of British Columbia and TRIUMF
Jan. 17, 2023
In this talk, I will examine the nuclear reactions 7Li(p,y)8Be and 7Li(p,e+e-)8Be from an ab initio perspective.Using chiral nucleon-nucleon and three-nucleon forces as input, the no-core shell model with continuum technique allows us to obtain an accurate description of both 8Be bound states and p+7Li scattering states.
The energy freed up by capture is enough to produce electron-positron pairs. The angular distribution of these pairs will be different if the intermediate particle is not the photon, for example, the axion or new vector or axial vector boson. Computing the standard model background and comparing experimental data with new decay modes is necessary to support or rule out new physics in the ATOMKI anomaly (which posits the existence of a new boson with a mass of 17 MeV).
Evan Rule
N3AS and University of California Berkeley
Dec 13, 2022
References: https://arxiv.org/abs/2203.09547, https://arxiv.org/abs/2208.07945, https://arxiv.org/abs/2109.13503
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Video Slides
Shohini Bhattacharya
Brookhaven National Laboratory
Dec 6, 2022
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Quark-Gluon matter from Holographic Black Holes
Joaquin Grefa
University of Houston
Nov. 15, 2022
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Luke Johns
University of California, Berkeley
Nov. 1, 2022
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Garrett King
Washington University
Oct. 18, 2022
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Qubit models, sign problems, and anomalies
Hersh Singh
InQubator for Quantum Simulation and Institute for Nuclear Theory
Oct. 18th, 2022
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