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The impact of cosmic ray feedback during the epoch of reionisation

Astronomy and Astrophysics 2025年第1期698卷

作者： Farcy, Marion Rosdahl, Joakim Dubois, Yohan Blaizot, Jérémy Martin-Alvarez, Sergio Haehnelt, Martin Kimm, Taysun Teyssier, Romain Institute of Physics Laboratory for Galaxy Evolution EPFL Observatoire de Sauverny Chemin Pegasi 51 Versoix1290 Switzerland Centre de Recherche Astrophysique de Lyon CNRS UMR 5574 Univ. Lyon Ens de Lyon 9 avenue Charles André Saint-Genis-LavalF-69230 France Institut d'Astrophysique de Paris CNRS UMR 7095 Sorbonne Université 98 bis bd Arago Paris75014 France Stanford University StanfordCA94305 United States Kavli Institute for Cosmology and Institute of Astronomy Madingley Road CambridgeCB3 0HA United Kingdom Department of Astronomy Yonsei University 50 Yonsei-ro Seodaemun-gu Seoul03722 Korea Republic of Department of Astrophysical Sciences Princeton University Peyton Hall PrincetonNJ08544 United States Program in Applied and Computational Mathematics Princeton University Fine Hall Washington Road PrincetonNJ08544-1000 United States

Galaxies form and evolve via a multitude of complex physics. In this work, we investigate the role of cosmic ray (CR) feedback in galaxy evolution and reionisation, by examining its impact on the escape of ionising radiation from galaxies. For this purpose, we present two SPHINX cosmological radiation-magneto-hydrodynamics simulations, enabling, for the first time, a study of the impact of CR feedback on thousands of resolved galaxies during the Epoch of Reionisation (EoR). The simulations differ in their feedback prescriptions: one adopts a calibrated strong supernova (SN) feedback, while the other reduces the strength of SN feedback and includes CR feedback instead. We show that both regulate star formation and match observations of high-redshift UV luminosity functions to a reasonable extent, while also producing a similar amount of hydrogen ionising photons. In contrast to the model with strong SN feedback, the model with CRs lead to incomplete reionisation, which is in strong disagreement with observational estimates of the reionisation history. This is due to CR feedback shaping the ISM differently, filling with gas the low-density cavities carved by SN explosions. As a result, this reduces the escape of ionising photons, at any halo mass, and primarily in the close vicinity of the stars. Our study indicates that CR feedback regulates galaxy growth during the EoR, but negatively affects reionisation. This tension paves the way for the further exploration and refinement of existing galaxy formation and feedback models. Such improvements are crucial in capturing and understanding the process of reionisation and the underlying evolution of galaxies through cosmic time. © The Authors 2025.

关键词： Cosmic rays

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Structure-mining: Screening structure models by automated fitting to the atomic pair distribution function over large numbers of models

arXiv

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arXiv 2019年

作者： Yang, Long Juhás, Pavol Terban, Maxwell W. Billinge, Simon J.L. Department of Applied Physics and Applied Mathematics Columbia University New YorkNY10027 United States Computational Science Initiative Brookhaven National Laboratory UptonNY11973 United States Max Planck Institute for Solid State Research Heisenbergstrasse 1 Stuttgart70569 Germany Condensed Matter Physics and Materials Science Department Brookhaven National Laboratory UptonNY11973 United States

Here we present a new approach to obtain candidate structures from atomic pair distribution function (PDF) data in a highly automated way. It pulls from modern structural databases all the structures meeting the experimenter's search criteria and performs structure refinements on them without human intervention. It supports both x-ray and neutron PDFs. Tests on various material systems show the effectiveness and robustness of the algorithm in finding the correct atomic crystal structure. It works on crystalline and nanocrystalline materials including complex oxide nanoparticles and nanowires, low-symmetry structures, and complicated doped and magnetic materials. This approach could greatly reduce the traditional structure searching work and enable the possibility of high-throughput real-time auto analysis PDF experiments in the future. Copyright © 2019, The Authors. All rights reserved.

关键词： Crystal atomic structure

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Cosmological phase-space analysis of f(G)-theories of gravity

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Journal of High Energy Astrophysics 2025年 47卷

作者： Papagiannopoulos, Giannis Luongo, Orlando Leon, Genly Paliathanasis, Andronikos Department of Physics National & Kapodistrian University of Athens Zografou Campus GR Athens 157 73 Greece School of Science and Technology University of Camerino Via Madonna delle Carceri Camerino 62032 Italy Department of Nanoscale Science and Engineering University at Albany-SUNY Albany 12222 NY United States INAF - Osservatorio Astronomico di Brera Milano Italy Istituto Nazionale di Fisica Nucleare (INFN) Sezione di Perugia Perugia 06123 Italy Al-Farabi Kazakh National University Al-Farabi av. 71 Almaty 050040 Kazakhstan Departamento de Matemáticas Universidad Católica del Norte Avda. Angamos 0610 Casilla 1280 Antofagasta Chile Department of Mathematics Faculty of Applied Sciences Durban University of Technology Durban 4000 South Africa School for Data Science and Computational Thinking Department of Mathematical Sciences Stellenbosch University Stellenbosch 7602 South Africa

The impact of topological terms that modify the Hilbert-Einstein action is here explored by virtue of a further f(G) contribution. In particular, we investigate the phase-space stability and critical points of an equivalent scalar field representation that makes use of a massive field, whose potential is function of the topological correction. To do so, we introduce to the gravitational Action Integral a Lagrange multiplier and model the modified Friedmann equations by virtue of new non-dimensional variables. We single out dimensionless variables that permit a priori the Hubble rate change of sign, enabling regions in which the Hubble parameter either vanishes or becomes negative. In this respect, we thus analyze the various possibilities associated with a universe characterized by such topological contributions and find the attractors, saddle points and regions of stability, in general. The overall analysis is carried out considering the exponential potential first and then shifting to more complicated cases, where the underlying variables do not simplify. We compute the eigenvalues of our coupled differential equations and, accordingly, the stability of the system, in both a spatially-flat and non-flat universe. Quite remarkably, regardless of the spatial curvature, we show that a stable de Sitter-like phase that can model current time appears only a small fraction of the entire phase-space, suggesting that the model under exam is unlikely in describing the whole universe dynamics, i.e., the topological terms appear disfavored in framing the entire evolution of the universe. © 2025 The Author(s)

关键词： Equilibrium points f(G)-gravity Gauss-Bonnet

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Carbon enrichment in APOGEE disk stars as evidence of mass transfer in binaries

arXiv

引用

arXiv 2024年

作者： Foster, Steve Schiavon, Ricardo P. de Castro, Denise B. Lucatello, Sara Daher, Christine Penoyre, Zephyr Price-Whelan, Adrian Badenes, Carles Fernández-Trincado, J.G. García-Hernández, D.A. Holtzman, Jon Jönsson, Henrik Shetrone, Matthew Astrophysics Research Institute Liverpool John Moores University 146 Brownlow Hill LiverpoolL3 5RF United Kingdom Fundação Getúlio Vargas RJ Rio de Janeiro22250-900 Brazil INAF Osservatorio Astronomico di Padova vicolo dell’Osservatorio 5 PadovaI-35122 Italy The Ohio State University 191 W. Woodruff Ave. ColumbusOH43206 United States Institute of Astronomy Madingley Rd CambridgeCB3 0HA United Kingdom Leiden Observatory Leiden University PO Box 9513 Leiden2300 RA Netherlands Center for Computational Astrophysics Flatiron Institute 162 5th Ave New YorkNY10010 United States Department of Physics and Astronomy University of Pittsburgh Allen Hall 3941 O’Hara St PittsburghPA15260 United States Instituto de Astronomía Universidad Católica del Norte Av. Angamos 0610 Antofagasta Chile Instituto de Astrofísica de Canarias Tenerife La Laguna38205 Spain Departamento de Astrofísica Tenerife La LagunaE-38206 Spain Department of Astronomy New Mexico State University PO BOX 30001 Las CrucesNM88003 United States Materials Science and Applied Mathematics Malmö University MalmöSE-205 06 Sweden University of California Observatories University of California Santa Cruz Santa CruzCA95064 United States

Context. Carbon abundances in first-ascent giant stars are usually lower than those of their main-sequence counterparts. At moderate metallicities, stellar evolution of single stars cannot account for the existence of red-giant branch stars with enhanced carbon abundances. The phenomenon is usually interpreted as resulting from past mass transfer from an evolved binary companion now in the white dwarf evolutionary stage. Aims. We aim to confirm the links between [C/O] enhancement, s−process element enhancement and binary fraction using large-scale catalogues of stellar abundances and probable binary stars. Methods. We use a large data set from the 17th data release of the SDSS-IV/APOGEE 2 survey to identify carbon-enhanced stars in the Galactic disk. We identify a continuum of carbon enrichment throughout three different sub-populations of disk stars and explore links between the degree of carbon enrichment and binary frequency, metallicity and chemical compositions. Results. We verify a clear correlation between binary frequency and enhancement in the abundances of both carbon and cerium, lending support to the scenario whereby carbon-enhanced stars are the result of mass transfer by an evolved binary companion. In addition, we identify clustering in the carbon abundances of high-α disk stars, suggesting that those on the high metallicity end are likely younger, in agreement with theoretical predictions for the presence of a starburst population following the gas-rich merger of the Gaia-Enceladus/Sausage system. Copyright © 2024, The Authors. All rights reserved.

关键词： White dwarfs

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Probing diffuse gas with fast radio bursts

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Physical Review D 2019年第10期100卷 103519-103519页

作者： Anthony Walters Yin-Zhe Ma Jonathan Sievers Amanda Weltman School of Chemistry and Physics University of KwaZulu-Natal Durban 4000 South Africa NAOC-UKZN Computational Astrophysics Centre (NUCAC) University of KwaZulu-Natal Durban 4000 South Africa Department of Physics and McGill Space Institute McGill University Montreal Quebec H3A 2T8 Canada The Cosmology and Gravity Group Department of Mathematics and Applied Mathematics University of Cape Town Private Bag Rondebosch 7700 Cape Town South Africa

The dispersion measure—redshift relation of fast radio bursts (FRBs), DM(z), has been proposed as a potential new probe of the cosmos, complementary to existing techniques. In practice, however, the effectiveness of this approach depends on a number of factors, including (but not limited to) the intrinsic scatter in the data caused by intervening matter inhomogeneities. Here, we simulate a number of catalogues of mock FRB observations, and use Markov Chain Monte Carlo techniques to forecast constraints, and assess which parameters will likely be best constrained. In all cases, we find that any potential improvement in cosmological constraints are limited by the current uncertainty on the diffuse gas fraction, fd(z). Instead, we find that the precision of current cosmological constraints allows one to constrain fd(z) and possibly its redshift evolution. Combining Cosmic Microwave Background + Baryon Acoustic Oscillations + Supernovae + H0 constraints with just 100 FRBs (with redshifts), we find a typical constraint on the mean diffuse gas fraction of a few percent. A detection of this nature would alleviate the “missing baryon problem,” and therefore highlights the value of localization and spectroscopic follow-up of future FRB detections.

关键词： Cosmological parameters Radio, microwave, & sub-mm astronomy Transient & explosive astronomical phenomena Intergalactic medium Large scale structure of the Universe Distances, redshifts, & velocities Astrophysical & cosmological simulations Electromagnetic radiation astronomy

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Strong modification of radiative transition rates due to a breit-interaction-induced avoided crossing

arXiv

引用

arXiv 2019年

作者： Hu, Zhimin Xiong, Gang Gao, Xiang Nakamura, Nobuyuki Yao, Ke Wu, Chengsheng Numadate, Naoki Huang, Chengwu Ma, Yulong Wu, Yong Li, Yueming Zou, Yaming Zhang, Baohan Yang, Jiamin Laser Fusion Research Center China Academy of Engineering Physics Mianyang621900 China Beijing Computational Science Research Center Beijing100084 China Institute for Theoretical Physics Vienna University of Technology ViennaA-1040 Austria Institute for Laser Science University of Electro-Communications Tokyo182-8585 Japan Fudan University Shanghai200433 China Department of Engineering Physics Tsinghua University Beijing100084 China Institute for Applied Physics and Computational Mathematics Beijing100088 China

We present the observations of x-rays emitted from the 1s2s22p1/22p3/2 inner shell excited state of B-like W and Bi ions. The relative transition rates are obtained for two dominant radiative transitions to 1s22s22p1/2 and 1s22s22p3/2. The experimental results and the comparison with rigorous relativistic calculations show that the rates of the strong electric dipole allowed 1s22s22p - 1s2s22p2 transitions are strongly modified due to a drastic change in the wavefunction caused by the Breit interaction. Copyright © 2019, The Authors. All rights reserved.

关键词： Excited states

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Multimuons in cosmic-ray events as seen in ALICE at the LHC

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Journal of Cosmology and Astroparticle physics 2025年第4期2025卷 009-009页

作者： Acharya, S. Agarwal, A. Aglieri Rinella, G. Aglietta, L. Agnello, M. Agrawal, N. Ahammed, Z. Ahmad, S. Ahn, S.U. Ahuja, I. Akindinov, A. Akishina, V. Al-Turany, M. Aleksandrov, D. Alessandro, B. Alfanda, H.M. Alfaro Molina, R. Ali, B. Alici, A. Alizadehvandchali, N. Alkin, A. Alme, J. Alocco, G. Alt, T. Altamura, A.R. Altsybeev, I. Alvarado, J.R. Alvarez, C.O.R. Anaam, M.N. Andrei, C. Andreou, N. Andronic, A. Andronov, E. Anguelov, V. Antinori, F. Antonioli, P. Apadula, N. Aphecetche, L. Appelshäuser, H. Arata, C. Arcelli, S. Arnaldi, R. Arneiro, J.G.M.C.A. Arsene, I.C. Arslandok, M. Augustinus, A. Averbeck, R. Averyanov, D. Azmi, M.D. Baba, H. Badalà, A. Bae, J. Bae, Y. Baek, Y.W. Bai, X. Bailhache, R. Bailung, Y. Bala, R. Balbino, A. Baldisseri, A. Balis, B. Banoo, Z. Barbasova, V. Barile, F. Barioglio, L. Barlou, M. Barman, B. Barnaföldi, G.G. Barnby, L.S. Barreau, E. Barret, V. Barreto, L. Bartels, C. Barth, K. Bartsch, E. Bastid, N. Basu, S. Batigne, G. Battistini, D. Batyunya, B. Bauri, D. Bazo Alba, J.L. Bearden, I.G. Beattie, C. Becht, P. Behera, D. Belikov, I. Bell Hechavarria, A.D.C. Bellini, F. Bellwied, R. Belokurova, S. Beltran, L.G.E. Beltran, Y.A.V. Bencedi, G. Bensaoula, A. Beole, S. Berdnikov, Y. Berdnikova, A. Bergmann, L. Besoiu, M.G. Betev, L. Bhaduri, P.P. Bhasin, A. Bhattacharjee, B. Bianchi, L. Bielčík, J. Bielčíková, J. Bigot, A.P. Bilandzic, A. Biro, G. Biswas, S. Bize, N. Blair, J.T. Blau, D. Blidaru, M.B. Bluhme, N. Blume, C. Bock, F. Bodova, T. Bok, J. Boldizsár, L. Bombara, M. Bond, P.M. Bonomi, G. Borel, H. Borissov, A. Borquez Carcamo, A.G. Botta, E. Bouziani, Y.E.M. Bratrud, L. Braun-Munzinger, P. Bregant, M. Broz, M. Bruno, G.E. Buchakchiev, V.D. Buckland, M.D. Budnikov, D. Buesching, H. Bufalino, S. Buhler, P. Burmasov, N. Buthelezi, Z. Bylinkin, A. Bysiak, S.A. Cabanillas Noris, J.C. Cabrera, M.F.T. Caines, H. Caliva, A. Calvo Villar, E. Camacho, J.M.M. Camerini, P. Canedo, F.D.M. Cantway, S.L. Carabas, M. Carballo, A.A. Carnesecchi, F. Caron, R. Carvalho, L.A.D. Castillo Castel A.I. Alikhanyan National Science Laboratory (Yerevan Physics Institute) Foundation Yerevan Armenia AGH University of Krakow Cracow Poland Bogolyubov Institute for Theoretical Physics National Academy of Sciences of Ukraine Kiev Ukraine Bose Institute Department of Physics Centre for Astroparticle Physics and Space Science (CAPSS) Kolkata India California Polytechnic State University San Luis Obispo CA United States Central China Normal University Wuhan China Centro de Aplicaciones Tecnológicas y Desarrollo Nuclear (CEADEN) Havana Cuba Centro de Investigación y de Estudios Avanzados (CINVESTAV) Mérida Mexico City Mexico Chicago State University Chicago IL United States China Institute of Atomic Energy Beijing China China University of Geosciences Wuhan China Chungbuk National University Cheongju South Korea Comenius University Bratislava Faculty of Mathematics Physics and Informatics Bratislava Slovakia Creighton University Omaha NE United States Department of Physics Aligarh Muslim University Aligarh India Department of Physics Pusan National University Pusan South Korea Department of Physics Sejong University Seoul South Korea Department of Physics University of California Berkeley CA United States Department of Physics University of Oslo Oslo Norway Department of Physics and Technology University of Bergen Bergen Norway Dipartimento di Fisica Università di Pavia Pavia Italy Dipartimento di Fisica dell’Università Sezione INFN Cagliari Italy Dipartimento di Fisica dell’Università Sezione INFN Trieste Italy Dipartimento di Fisica dell’Università Sezione INFN Turin Italy Dipartimento di Fisica e Astronomia dell’Università Sezione INFN Bologna Italy Dipartimento di Fisica e Astronomia dell’Università Sezione INFN Catania Italy Dipartimento di Fisica e Astronomia dell’Università Sezione INFN Padova Italy Dipartimento di Fisica ‘E.R. Caianiello’ dell’Università Gruppo Collegato INFN Salerno Italy Dipartimento DISAT del Politecnico Sezione

ALICE is a large experiment at the CERN Large Hadron Collider. Located 52 meters underground, its detectors are suitable to measure muons produced by cosmic-ray interactions in the atmosphere. In this paper, the studies of the cosmic muons registered by ALICE during Run 2 (2015–2018) are described. The analysis is limited to multimuon events defined as events with more than four detected muons (N_µ > 4) and in the zenith angle range 0^◦ < θ < 50^◦. The results are compared with Monte Carlo simulations using three of the main hadronic interaction models describing the air shower development in the atmosphere: QGSJET-II-04, EPOS-LHC, and SIBYLL 2.3d. The interval of the primary cosmic-ray energy involved in the measured muon multiplicity distribution is about 4×10¹⁵ < E_prim < 6×10¹⁶ eV. In this interval none of the three models is able to describe precisely the trend of the composition of cosmic rays as the energy increases. However, QGSJET-II-04 is found to be the only model capable of reproducing reasonably well the muon multiplicity distribution, assuming a heavy composition of the primary cosmic rays over the whole energy range, while SIBYLL 2.3d and EPOS-LHC underpredict the number of muons in a large interval of multiplicity by more than 20% and 30%, respectively. The rate of high muon multiplicity events (N_µ > 100) obtained with QGSJET-II-04 and SIBYLL 2.3d is compatible with the data, while EPOS-LHC produces a significantly lower rate (55% of the measured rate). For both QGSJET-II-04 and SIBYLL 2.3d, the rate is close to the data when the composition is assumed to be dominated by heavy elements, an outcome compatible with the average energy E_prim ∼ 10¹⁷ eV of these events. This result places significant constraints on more exotic production mechanisms. © 2025 The Author(s).

关键词： cosmic ray experiments cosmic rays detectors

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Void distributions reveal structural link between jammed packings and protein cores

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Physical Review E 2019年第2期99卷 022416-022416页

作者： John D. Treado Zhe Mei Lynne Regan Corey S. O'Hern Department of Mechanical Engineering & Materials Science Yale University New Haven Connecticut 06520 USA Integrated Graduate Program in Physical & Engineering Biology Yale University New Haven Connecticut 06520 USA Department of Chemistry Yale University New Haven Connecticut 06520 USA Department of Molecular Biophysics & Biochemistry Yale University New Haven Connecticut 06520 USA Department of Physics Yale University New Haven Connecticut 06520 USA Department of Applied Physics Yale University New Haven Connecticut 06520 USA Program in Computational Biology and Bioinformatics Yale University New Haven Connecticut 06520 USA

Dense packing of hydrophobic residues in the cores of globular proteins determines their stability. Recently, we have shown that protein cores possess packing fraction ϕ≈0.56, which is the same as dense, random packing of amino-acid-shaped particles. In this article, we compare the structural properties of protein cores and jammed packings of amino-acid-shaped particles in much greater depth by measuring their local and connected void regions. We find that the distributions of surface Voronoi cell volumes and local porosities obey similar statistics in both systems. We also measure the probability that accessible, connected void regions percolate as a function of the size of a spherical probe particle and show that both systems possess the same critical probe size. We measure the critical exponent τ that characterizes the size distribution of connected void clusters at the onset of percolation. We find that the cluster size statistics are similar for void percolation in packings of amino-acid-shaped particles and randomly placed spheres, but different from that for void percolation in jammed sphere packings. We propose that the connected void regions are a defining structural feature of proteins and can be used to differentiate experimentally observed proteins from decoy structures that are generated using computational protein design software. This work emphasizes that jammed packings of amino-acid-shaped particles can serve as structural and mechanical analogs of protein cores, and could therefore be useful in modeling the response of protein cores to cavity-expanding and -reducing mutations.

关键词： Jamming Protein structure Packing & jamming problems Proteins Crystal structures Finite-size scaling Molecular dynamics Percolation theory

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MONGE-AMPÈRE FLOW FOR GENERATIVE MODELING

arXiv

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arXiv 2018年

作者： Zhang, Linfeng Weinan, E. Wang, Lei Program in Applied and Computational Mathematics Princeton University United States Department of Mathematics and Program in Applied and Computational Mathematics Princeton University United States Center for Data Science Peking University Beijing Institute of Big Data Research Beijing100871 China Institute of Physics Chinese Academy of Sciences Beijing100190 China

We present a deep generative model, named Monge-Ampère flow, which builds on continuous-time gradient flow arising from the Monge-Ampère equation in optimal transport theory. The generative map from the latent space to the data space follows a dynamical system, where a learnable potential function guides a compressible fluid to flow towards the target density distribution. Training of the model amounts to solving an optimal control problem. The Monge-Ampère flow has tractable likelihoods and supports efficient sampling and inference. One can easily impose symmetry constraints in the generative model by designing suitable scalar potential functions. We apply the approach to unsupervised density estimation of the MNIST dataset and variational calculation of the two-dimensional Ising model at the critical point. This approach brings insights and techniques from Monge-Ampère equation, optimal transport, and fluid dynamics into reversible flow-based generative models. Copyright © 2018, The Authors. All rights reserved.

关键词： Statistical mechanics

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First-principles study of solute diffusion in Ni3Al

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Chinese physics B 2017年第9期26卷 126-132页

作者：刘少华李孜王崇愚 School of Materials Science and Engineering Tsinghua UniversityBeijing 100084China Institute of Applied Physics and Computational Mathematics Beijing 100088China Department of Physics Tsinghua UniversityBeijing 100084China

Using first-principles calculations in combination with Wagner–Schottky and kinetic Monte Carlo methods, the diffusion behaviors of solutes via various vacancy-mediated diffusion mechanisms in L12 γ-Ni3Al were investigated. The formation energies of the point defects and the migration energies for solutes were calculated. Adding alloying elements can decrease the defect-formation energies of NiAl, increase the defect-formation energies of AlNi, and have little effect on the formation energy of VNi. The migration energies of solutes are related with the site preference and the diffusion mechanism. The diffusion coefficients of Ni, Al, and solutes were calculated, and the concentration of antisite defects plays a crucial role in the elemental diffusion.

关键词： nickel-based superalloy diffusion Ni3Al first-principles

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