检索结果-内蒙古大学图书馆

arXiv 2022年

作者： Abe, H. Adhikari, R.X. Akutsu, T. Ando, M. Araya, A. Aritomi, N. Asada, H. Aso, Y. Bae, S. Bae, Y. Bajpai, R. Ballmer, S.W. Cannon, K. Cao, Z. Capocasa, E. Chan, M. Chen, C. Chen, D. Chen, K. Chen, Y. Chiang, C-Y. Chu, Y-K. Driggers, J.C. Dwyer, S.E. Effler, A. Eguchi, S. Eisenmann, M. Enomoto, Y. Kokeyama, K. Washimi, Tatsuki Yamamoto, K. Graduate School Of Science Tokyo Institute Of Technology 2-12-1 Ookayama Meguro-ku Tokyo152-8551 Japan LIGO Laboratory California Institute Of Technology 1200 East California Boulevard PasadenaCA91125 United States 2-21-1 Osawa Mitaka City Tokyo181-8588 Japan 2-21-1 Osawa Mitaka City Tokyo181-8588 Japan Department Of Physics The University Of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo113-0033 Japan The University Of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo113-0033 Japan Earthquake Research Institute The University Of Tokyo 1-1-1 Yayoi Bunkyo-ku Tokyo113-0032 Japan Department Of Mathematics And Physics Hirosaki University Aomori Hirosaki036-8561 Japan 238 Higashi-Mozumi Kamioka-cho Hida City Gifu506-1205 Japan 2-21-1 Osawa Mitaka City Tokyo181-8588 Japan 245 Daehak-ro Yuseong-gu Daejeon34141 Korea Republic of National Institute For Mathematical Sciences 70 Yuseong-daero 1689 Beon-gil Yuseong-gu Daejeon34047 Korea Republic of 1-1 Oho Ibaraki Tsukuba305-0801 Japan Department Of Physics Syracuse University 900 South Crouse Ave. SyracuseNY13244 United States Department Of Astronomy Beijing Normal University Xinjiekouwai Street 19 Haidian District Beijing100875 China Laboratoire Astro Particulea And Cosmology Universite De Paris 10 rue Alice Domon et Leonie Duquet Paris75013 France Department Of Applied Physics Fukuoka University 8-19-1 Nanakuma Fukuoka City Fukuoka Jonan814-0180 Japan Department Of Physics Tamkang University No. 151 Yingzhuan Rd. Danshui Dist. New Taipei City25137 Taiwan Department Of Physics Institute Of Astronomy National Tsing Hua University No. 101 Section 2 Kuang-Fu Road Hsinchu30013 Taiwan Department Of Physics Center For High Energy And High Field Physics National Central University No.300 Zhongda Rd Zhongli District Taoyuan City32001 Taiwan Department Of Physics National Tsing Hua University No. 101 Section 2 Kuang-Fu Road Hsinchu30013 Taiwan Institute Of Physics Academia Si

KAGRA, the kilometer-scale underground gravitational-wave detector, is located at Kamioka, Japan. In April 2020, an astrophysics observation was performed at the KAGRA detector in combination with the GEO 600 detector;this observation operation is called O3GK. The optical configuration in O3GK is based on a power recycled Fabry-Pérot Michelson interferometer;all the mirrors were set at room temperature. The duty factor of the operation was approximately 53%, and the strain sensitivity was 3 × 10-22/ √ Hz at 250 Hz. In addition, the binary-neutron-star (BNS) inspiral range was approximately 0.6 Mpc. The contributions of various noise sources to the sensitivity of O3GK were investigated to understand how the observation range could be improved;this study is called a "noise budget." According to our noise budget, the measured sensitivity could be approximated by adding up the effect of each noise. The sensitivity was dominated by noise from the sensors used for local controls of the vibration isolation systems, acoustic noise, shot noise, and laser frequency noise. Further, other noise sources that did not limit the sensitivity were investigated. This paper provides a detailed account of the KAGRA detector in O3GK including interferometer configuration, status, and noise budget. In addition, strategies for future sensitivity improvements such as hardware upgrades, are discussed. © 2022, CC BY.

关键词： Shot noise

来源：评论

学校读者我要写书评

暂无评论

Plastic deformation transition in FeCrCoNiAl_x high-entropy alloys

引用

Materials Research Letters 2019年第11期7卷 439-445页

作者： Huang, Shuo Li, Wei Holmström, Erik Kwon, Se Kyun Eriksson, Olle Vitos, Levente Department of Physics and Astronomy Division of Materials Theory Uppsala University Uppsala Sweden Applied Materials Physics Department of Materials Science and Engineering Royal Institute of Technology Stockholm Sweden Sandvik Coromant R&D Stockholm Sweden Graduate Institute of Ferrous Technology Pohang University of Science and Technology Pohang South Korea School of Science and Technology Örebro University Örebro Sweden Institute for Solid State Physics and Optics Wigner Research Centre for Physics Budapest Hungary

The competition between plastic deformation mechanisms in FeCrCoNiAlx high-entropy alloys is explored as a function of temperature by first-principle theory. Investigating the generalized stacking fault energy, we ide... 详细信息

The competition between plastic deformation mechanisms in FeCrCoNiAl_x high-entropy alloys is explored as a function of temperature by first-principle theory. Investigating the generalized stacking fault energy, we identify a strong interplay between the magnetic and chemical effects. At cryogenic conditions (ferromagnetic state), full-slip is accompanied by martensitic transformation, whereas increasing temperature towards room-temperature (paramagnetic state) changes the deformation mechanism to full-slip plus twinning. Alloying with Al reduces the susceptibility for stacking fault formation in the ferromagnetic state and promotes twinning in the paramagnetic state. The present advance in magneto-plasticity reveals new opportunities for tailoring the mechanical response in high-entropy alloys. IMPACT STATEMENT: Magnetic state critically affects the γ-surface of FeCrCoNiAl_x and is responsible for the emergence of the exceptional metastable twinning phenomena at room temperature. © 2019, © 2019 The Author(s). Published by Informa UK Limited, trading as Taylor & Francis Group.

关键词： ab initio calculations generalized stacking fault energy High-entropy alloys TWIP/TRIP effects

来源：评论

学校读者我要写书评

暂无评论

Characterization of Markarian 421 during its most violent year: Multiwavelength variability and correlations

arXiv

引用

arXiv 2025年

作者： Abe, K. Abe, S. Abhir, J. Abhishek, A. Acciari, V.A. Aguasca-Cabot, A. Agudo, I. Aniello, T. Ansoldi, S. Antonelli, L.A. Engels, A. Arbet Arcaro, C. Asano, K. Baack, D. Babić, A. de Almeida, U. Barres Barrio, J.A. Batković, I. Bautista, A. Baxter, J. González, J. Becerra Bednarek, W. Bernardini, E. Bernete, J. Berti, A. Besenrieder, J. Bigongiari, C. Biland, A. Blanch, O. Bonnoli, G. Bošnjak, Ž. Bronzini, E. Burelli, I. Campoy-Ordaz, A. Carosi, R. Carretero-Castrillo, M. Castro-Tirado, A.J. Cerasole, D. Ceribella, G. Chai, Y. Cifuentes, A. Colombo, E. Contreras, J.L. Cortina, J. Covino, S. D’Amico, G. D’Ammando, F. D’Elia, V. Da Vela, P. Dazzi, F. De Angelis, A. De Lotto, B. de Menezes, R. Delfino, M. Delgado, J. Mendez, C. Delgado Di Pierro, F. Di Tria, R. Di Venere, L. Prester, D. Dominis Donini, A. Dorner, D. Doro, M. Eisenberger, L. Elsaesser, D. Escudero, J. Fariña, L. Fattorini, A. Foffano, L. Font, L. Fröse, S. Fukami, S. Fukazawa, Y. López, R.J. García Garczarczyk, M. Gasparyan, S. Gaug, M. Paiva, J.G. Giesbrecht Giglietto, N. Giordano, F. Gliwny, P. Godinović, N. Gradetzke, T. Grau, R. Green, D. Green, J.G. Günther, P. Hadasch, D. Hahn, A. Hassan, T. Heckmann, L. Llorente, J. Herrera Hrupec, D. Imazawa, R. Ishio, K. Martínez, I. Jiménez Jormanainen, J. Kankkunen, S. Kayanoki, T. Kerszberg, D. Kluge, G.W. Kouch, P.M. Kubo, H. Kushida, J. Láinez, M. Lamastra, A. Leone, F. Lindfors, E. Lombardi, S. Longo, F. López-Coto, R. López-Moya, M. López-Oramas, A. Loporchio, S. Lorini, A. Majumdar, P. Makariev, M. Maneva, G. Manganaro, M. Mangano, S. Mannheim, K. Mariotti, M. Martínez, M. Martínez-Chicharro, M. Mas-Aguilar, A. Mazin, D. Menchiari, S. Mender, S. Miceli, D. Miener, T. Miranda, J.M. Mirzoyan, R. González, M. Molero Molina, E. Mondal, H.A. Moralejo, A. Morcuende, D. Nakamori, T. Nanci, C. Neustroev, V. Nickel, L. Nigro, C. Nikolić, L. Nilsson, K. Nishijima, K. Ekoume, T. Njoh Noda, K. Nozaki, S. Okumura, A. Otero-Santos, J. Paiano, S. Japanese MAGIC Group Department of Physics Tokai University Kanagawa Hiratsuka259-1292 Japan The University of Tokyo Chiba Kashiwa277-8582 Japan ETH Zürich ZürichCH-8093 Switzerland Università di Siena INFN Pisa SienaI-53100 Italy Bellaterra BarcelonaE-08193 Spain Universitat de Barcelona ICCUB IEEC-UB BarcelonaE-08028 Spain Instituto de Astrofísica de Andalucía-CSIC Glorieta de la Astronomía s/n Granada18008 Spain RomeI-00136 Italy Università di Udine INFN Trieste UdineI-33100 Italy Max-Planck-Institut für Physik GarchingD-85748 Germany Università di Padova INFN PadovaI-35131 Italy Technische Universität Dortmund DortmundD-44221 Germany Zagreb10000 Croatia URCA RJ Rio de Janeiro22290-180 Brazil IPARCOS Institute EMFTEL Department Universidad Com-plutense de Madrid MadridE-28040 Spain Instituto de Astrofísica de Canarias Dpto. de Astrofísica Universidad de La Laguna La Laguna TenerifeE-38200 Spain University of Lodz Faculty of Physics and Applied Informatics Department of Astrophysics Lodz90-236 Poland Centro de Investigaciones Energéticas Medioambientales y Tecnológicas MadridE-28040 Spain Departament de Física CERES-IEEC Universitat Autònoma de Barcelona BellaterraE-08193 Spain Università di Pisa INFN Pisa PisaI-56126 Italy INFN MAGIC Group INFN Sezione di Bari Dipartimento Interateneo di Fisica dell’Università e del Politecnico di Bari BariI-70125 Italy Department for Physics and Technology University of Bergen Norway INFN MAGIC Group INFN Sezione di Torino Università degli Studi di Torino TorinoI-10125 Italy Croatian MAGIC Group University of Rijeka Faculty of Physics Rijeka51000 Croatia Universität Würzburg WürzburgD-97074 Germany Japanese MAGIC Group: Physics Program Graduate School of Advanced Science and Engineering Hiroshima University Hiroshima739-8526 Japan ZeuthenD-15738 Germany Armenian MAGIC Group: ICRANet-Armenia Yerevan0019 Armenia Split21000 Croatia Croatian MAGIC Group J

Aims. Mrk 421 was in its most active state around early 2010, which led to the highest TeV gamma-ray flux ever recorded from any active galactic nuclei (AGN). We aim to characterize the multiwavelength behavior during this exceptional year for Mrk 421, and evaluate whether it is consistent with the picture derived with data from other less exceptional years. Methods. We investigated the period from November 5, 2009, (MJD 55140) until July 3, 2010, (MJD 55380) with extensive coverage from very-high-energy (VHE;E > 100 GeV) gamma rays to radio with MAGIC, VERITAS, Fermi-LAT, RXTE, Swift, GASP-WEBT, VLBA, and a variety of additional optical and radio telescopes. We characterized the variability by deriving fractional variabilities as well as power spectral densities (PSDs). In addition, we investigated images of the jet taken with VLBA and the correlation behavior among different energy bands. Results. Mrk 421 was in widely different states of activity throughout the campaign, ranging from a low-emission state to its highest VHE flux ever recorded. We find the strongest variability in X-rays and VHE gamma rays, and PSDs compatible with power-law functions with indices around 1.5. We observe strong correlations between X-rays and VHE gamma rays at zero time lag with varying characteristics depending on the exact energy band. We also report a marginally significant (∼ 3σ) positive correlation between high-energy (HE;E > 100 MeV) gamma rays and the ultraviolet band. We detected marginally significant (∼ 3σ) correlations between the HE and VHE gamma rays, and between HE gamma rays and the X-ray, that disappear when the large flare in February 2010 is excluded from the correlation study, hence indicating the exceptionality of this flaring event in comparison with the rest of the campaign. The 2010 violent activity of Mrk421 also yielded the first ejection of features in the VLBA images of the jet of Mrk 421. Yet the large uncertainties in the ejection times of these unprece

关键词： Active Galactic Nuclei

来源：评论

学校读者我要写书评

暂无评论

Empowering Precision Medicine: AI-Driven Schizophrenia Diagnosis via EEG Signals: A Comprehensive Review from 2002-2023

arXiv

引用

arXiv 2023年

作者： Jafari, Mahboobeh Sadeghi, Delaram Shoeibi, Afshin Alinejad-Rokny, Hamid Beheshti, Amin García, David López Chen, Zhaolin Acharya, U. Rajendra Gorriz, Juan M. Internship in BioMedical Machine Learning Lab The Graduate School of Biomedical Engineering UNSW Sydney SydneyNSW2052 Australia Data Science and Computational Intelligence Institute University of Granada Spain BioMedical Machine Learning Lab The Graduate School of Biomedical Engineering UNSW Sydney SydneyNSW2052 Australia UNSW Data Science Hub The University of New South Wales SydneyNSW2052 Australia Health Data Analytics Program Centre for Applied Artificial Intelligence Macquarie University Sydney2109 Australia Data Science Lab School of Computing Macquarie University SydneyNSW2109 Australia Monash University Melbourne Australia School of Mathematics Physics and Computing University of Southern Queensland Springfield Australia Department of Psychiatry University of Cambridge United Kingdom

Schizophrenia (SZ) is a prevalent mental disorder characterized by cognitive, emotional, and behavioral changes. Symptoms of SZ include hallucinations, illusions, delusions, lack of motivation, and difficulties in concentration. While the exact causes of SZ remain unproven, factors such as brain injuries, stress, and psychotropic drugs have been implicated in its development. SZ can be classified into different types, including paranoid, disorganized, catatonic, undifferentiated, and residual. Diagnosing SZ involves employing various tools, including clinical interviews, physical examinations, psychological evaluations, the Diagnostic and Statistical Manual of Mental Disorders (DSM), and neuroimaging techniques. Electroencephalography (EEG) recording is a significant functional neuroimaging modality that provides valuable insights into brain function during SZ. However, EEG signal analysis poses challenges for neurologists and scientists due to the presence of artifacts, long-term recordings, and the utilization of multiple channels. To address these challenges, researchers have introduced artificial intelligence (AI) techniques, encompassing conventional machine learning (ML) and deep learning (DL) methods, to aid in SZ diagnosis. This study reviews papers focused on SZ diagnosis utilizing EEG signals and AI methods. The introduction section provides a comprehensive explanation of SZ diagnosis methods and intervention techniques. Subsequently, review papers in this field are discussed, followed by an introduction to the AI methods employed for SZ diagnosis and a summary of relevant papers presented in tabular form. Additionally, this study reports on the most significant challenges encountered in SZ diagnosis, as identified through a review of papers in this field. Future directions to overcome these challenges are also addressed. The discussion section examines the specific details of each paper, culminating in the presentation of conclusions and findings. © 2023,

关键词： Electroencephalography

来源：评论

学校读者我要写书评

暂无评论

Constraints on axion-like particles with the Perseus Galaxy Cluster with MAGIC

arXiv

引用

arXiv 2024年

作者： Abe, H. Abe, S. Abhir, J. Acciari, V.A. Agudo, I. Aniello, T. Ansoldi, S. Antonelli, L.A. Engels, A. Arbet Arcaro, C. Artero, M. Asano, K. Baack, D. Babić, A. Baquero, A. de Almeida, U. Barres Barrio, J.A. Batković, I. Baxter, J. González, J. Becerra Bednarek, W. Bernardini, E. Bernete, J. Berti, A. Besenrieder, J. Bigongiari, C. Biland, A. Blanch, O. Bonnoli, G. Bošnjak, Ž. Burelli, I. Busetto, G. Campoy-Ordaz, A. Carosi, A. Carosi, R. Carretero-Castrillo, M. Castro-Tirado, A.J. Ceribella, G. Chai, Y. Cifuentes, A. Cikota, S. Colombo, E. Contreras, J.L. Cortina, J. Covino, S. D’Amico, G. D’Elia, V. Da Vela, P. Dazzi, F. De Angelis, A. De Lotto, B. Del Popolo, A. Delgado, J. Mendez, C. Delgado Depaoli, D. Di Pierro, F. Di Venere, L. Prester, D. Dominis Donini, A. Dorner, D. Doro, M. Elsaesser, D. Emery, G. Escudero, J. Fariña, L. Fattorini, A. Foffano, L. Font, L. Fukami, S. Fukazawa, Y. López, R.J. García Garczarczyk, M. Gasparyan, S. Gaug, M. Paiva, J.G. Giesbrecht Giglietto, N. Giordano, F. Gliwny, P. Godinović, N. Grau, R. Green, D. Green, J.G. Hadasch, D. Hahn, A. Hassan, T. Heckmann, L. Herrera, J. Hrupec, D. Hütten, M. Imazawa, R. Inada, T. Iotov, R. Ishio, K. Martínez, I. Jiménez Jormanainen, J. Kerszberg, D. Kluge, G.W. Kobayashi, Y. Kouch, P.M. Kubo, H. Kushida, J. Lezáun, M. Láinez Lamastra, A. Leone, F. Lindfors, E. Linhoff, L. Lombardi, S. Longo, F. López-Coto, R. López-Moya, M. López-Oramas, A. Loporchio, S. Lorini, A. de Oliveira Fraga, B. Machado Majumdar, P. Makariev, M. Maneva, G. Mang, N. Manganaro, M. Mangano, S. Mannheim, K. Mariotti, M. Martínez, M. Martínez-Chicharro, M. Mas-Aguilar, A. Mazin, D. Menchiari, S. Mender, S. Miceli, D. Miener, T. Miranda, J.M. Mirzoyan, R. González, M. Molero Molina, E. Mondal, H.A. Moralejo, A. Morcuende, D. Nakamori, T. Nanci, C. Nava, L. Neustroev, V. Nickel, L. Rosillo, M. Nievas Nigro, C. Nikolić, L. Nilsson, K. Nishijima, K. Ekoume, T. Njoh Noda, K. Nozaki, S. Ohtani, Y. Okumura, A. The University of Tokyo Chiba Kashiwa277-8582 Japan ETH Zürich ZürichCH-8093 Switzerland Instituto de Astrofísica de Canarias Dpto. de Astrofísica Universidad de La Laguna Tenerife La LagunaE-38200 Spain Instituto de Astrofísica de Andalucía-CSIC Glorieta de la Astronomía s/n Granada18008 Spain RomeI-00136 Italy Università di Udine INFN Trieste UdineI-33100 Italy Max-Planck-Institut für Physik MünchenD-80805 Germany Università di Padova INFN PadovaI-35131 Italy Bellaterra BarcelonaE-08193 Spain Technische Universität Dortmund DortmundD-44221 Germany Zagreb10000 Croatia IPARCOS Institute EMFTEL Department Universidad Complutense de Madrid MadridE-28040 Spain URCA RJ Rio de Janeiro22290-180 Brazil University of Lodz Faculty of Physics and Applied Informatics Department of Astrophysics Lodz90-236 Poland Centro de Investigaciones Energéticas Medioambientales y Tecnológicas MadridE-28040 Spain Departament de Física CERES-IEEC Universitat Autònoma de Barcelona BellaterraE-08193 Spain Università di Pisa INFN Pisa PisaI-56126 Italy Universitat de Barcelona ICCUB IEEC-UB BarcelonaE-08028 Spain Department for Physics and Technology University of Bergen Norway INFN MAGIC Group INFN Sezione di Catania Dipartimento di Fisica e Astronomia University of Catania CataniaI-95123 Italy INFN MAGIC Group INFN Sezione di Torino Università degli Studi di Torino TorinoI-10125 Italy INFN MAGIC Group INFN Sezione di Bari Dipartimento Interateneo di Fisica Università e del Politecnico di Bari BariI-70125 Italy Croatian MAGIC Group University of Rijeka Faculty of Physics Rijeka51000 Croatia University of Geneva Chemin d’Ecogia 16 VersoixCH-1290 Switzerland Japanese MAGIC Group Physics Program Graduate School of Advanced Science and Engineering Hiroshima University Hiroshima739-8526 Japan ZeuthenD-15738 Germany Armenian MAGIC Group ICRANet-Armenia Yerevan0019 Armenia Split21000 Croatia Croatian MAGIC Group Josip Jura

Axion-like particles (ALPs) are pseudo-Nambu-Goldstone bosons that emerge in various theories beyond the standard model. These particles can interact with high-energy photons in external magnetic fields, influencing the observed gamma-ray spectrum. This study analyzes 41.3 hrs of observational data from the Perseus Galaxy Cluster collected with the MAGIC telescopes. We focused on the spectra the radio galaxy in the center of the cluster: NGC 1275. By modeling the magnetic field surrounding this target, we searched for spectral indications of ALP presence. Despite finding no statistical evidence of ALP signatures, we were able to exclude ALP models in the sub-micro electronvolt range. Our analysis improved upon previous work by calculating the full likelihood and statistical coverage for all considered models across the parameter space. Consequently, we achieved the most stringent limits to date for ALP masses around 50 neV, with cross sections down to gaγ = 3 × 10−12 GeV−1 Copyright © 2024, The Authors. All rights reserved.

关键词： Gamma rays

来源：评论

学校读者我要写书评

暂无评论

Gamma-ray Bursts as Distance Indicators by a Statistical Learning Approach

arXiv

引用

arXiv 2024年

作者： Dainotti, Maria Giovanna Narendra, Aditya Pollo, Agnieszka Petrosian, Vahé Bogdan, Malgorzata Iwasaki, Kazunari Prochaska, Jason Xavier Rinaldi, Enrico Zhou, David National Astronomical Observatory of Japan Mitaka Tokyo181-8588 Japan The Graduate University for Advanced Studies SOKENDAI Kanagawa240-0193 Japan Space Science Institute BoulderCO80301 United States Doctoral School of Exact and Natural Sciences Jagiellonian University Krakow Poland Astronomical Observatory of Jagiellonian University Krakow Poland Warsaw Poland Department of Physics Stanford University 382 Via Pueblo Mall StanfordCA94305-4060 United States Kavli Institute for Particle Astrophysics and Cosmology Stanford University United States Department of Applied Physics Stanford University United States Department of Mathematics University of Wroclaw 50-384 Poland Department of Statistics Lund University LundSE-221 00 Sweden Center for Computational Astrophysics National Astronomical Observatory of Japan 2 Chome-21-1 Osawa Mitaka Tokyo181-8588 Japan University of California Santa Cruz 1156 High Street Santa CruzCA95064 United States Program RIKEN Saitama Wakoshi 351-0198 Japan Arizona State University 1151 S Forest Ave TempeAZ85281 United States

Gamma-ray bursts (GRBs) can be probes of the early universe, but currently, only 26% of GRBs observed by the Neil Gehrels Swift Observatory GRBs have known redshifts (z) due to observational limitations. To address this, we estimated the GRB redshift (distance) via a supervised statistical learning model that uses optical afterglow observed by Swift and ground-based telescopes. The inferred redshifts are strongly correlated (a Pearson coefficient of 0.93) with the observed redshifts, thus proving the reliability of this method. The inferred and observed redshifts allow us to estimate the number of GRBs occurring at a given redshift (GRB rate) to be 8.47-9yr−1Gpc−1 for 1.9 © 2024, CC BY.

关键词： Stars

来源：评论

学校读者我要写书评

暂无评论

Overcoming the surface paradox: Buried perovskite quantum dots in wide-bandgap perovskite thin films

arXiv

引用

arXiv 2025年

作者： Zhang, Hao Pasha, Altaf Metcalf, Isaac Zhou, Jianlin Staunstrup, Mathias Zhu, Yunxuan Liao, Shusen Ssennyimba, Ken Chen, Jia-Shiang Reddy, Surya Prakash Thébaud, Simon Hou, Jin Shuai, Xinting Mandani, Faiz Sidhik, Siraj Jones, Matthew R. Ma, Xuedan Balakrishna, R. Geetha Susarla, Sandhya Ginger, David S. Katan, Claudine Kanatzidis, Mercouri G. Bawendi, Moungi G. Natelson, Douglas Tamarat, Philippe Lounis, Brahim Even, Jacky Mohite, Aditya D. Department of Chemical and Biomolecular Engineering Rice University HoustonTX77005 United States Applied Physics Program Smalley‐Curl Institute Rice University HoustonTX77005 United States Centre for Nano and Material Sciences Jain University Jain Global Campus Kanakapura Karnataka Bangalore562112 India Department of Materials Science and NanoEngineering Rice University HoustonTX77005 United States Université de Bordeaux LP2N Talence France Institut d’Optique CNRS LP2N Talence France Department of Physics and Astronomy Rice University HoustonTX77005 United States Center for Nanoscale Materials Argonne National Laboratory LemontIL60439 United States School for Engineering of Matter Transport and Energy Arizona State University TempeAZ85281 United States UMR 6082 CNRS INSA de Rennes Rennes35708 France Department of Chemistry Rice University HoustonTX77005 United States Department of Chemistry University of Washington Box 351700 SeattleWA98195-1700 United States UMR 6226 Rennes35000 France Department of Chemistry Northwestern University EvanstonIL United States Department of Chemistry Massachusetts Institute of Technology 77 Massachusetts Avenue CambridgeMA02139 United States Department of Electrical and Computer Engineering Rice University HoustonTX77005 United States

Colloidal perovskite quantum dots (PQDs) are an exciting platform for on-demand quantum, and classical optoelectronic and photonic devices. However, their potential success is limited by the extreme sensitivity and low stability arising from their weak intrinsic lattice bond energy and complex surface chemistry. Here we report a novel platform of buried perovskite quantum dots (b-PQDs) in a three-dimensional perovskite thin-film, fabricated using one-step, flash annealing, which overcomes surface related instabilities in colloidal perovskite dots. The b-PQDs demonstrate ultrabright and stable single-dot emission, with resolution-limited linewidths below 130 μeV, photon-antibunching (g2(0)=0.1), no blinking, suppressed spectral diffusion, and high photon count rates of 104/s, consistent with unity quantum yield. The ultrasharp linewidth resolves exciton fine-structures (dark and triplet excitons) and their dynamics under a magnetic field. Additionally, b-PQDs can be electrically driven to emit single photons with 1 meV linewidth and photon-antibunching (g2(0)=0.4). These results pave the way for on-chip, low-cost single-photon sources for next generation quantum optical communication and sensing. © 2025, CC BY.

关键词： Photons

来源：评论

学校读者我要写书评

暂无评论

Unique chemical composition of the very metal-poor star LAMOST J1645+4357

arXiv

引用

arXiv 2023年

作者： Aoki, Wako Li, Haining Tominaga, Nozomu Matsuno, Tadafumi Honda, Satoshi Zhao, Gang National Astronomical Observatory of Japan National Institutes of Natural Sciences 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Astronomical Science Program Graduate Institute for Advanced Studies SOKENDAI 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Key Lab of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences A20 Datun Road Chaoyang Beijing100012 China Department of Physics Faculty of Science and Engineering Konan University 8-9-1 Okamoto Hyogo Kobe658-8501 Japan Kapteyn Astronomical Institute University of Groningen Landleven 12 Groningen9747 AD Netherlands Nishi-Harima Astronomical Observatory Center for Astronomy University of Hyogo 407-2 Nishigaichi Sayo-cho Hyogo Sayo679-5313 Japan

We report on the chemical composition of the very metal-poor ([Fe/H]= −2.9) star LAMOST J1645+4357 that is identified to be a red giant having peculiar abundance ratios by Li et al. (2022). The standard abundance analysis is carried out for this object and the well studied metal-poor star HD 122563 that has similar atmospheric parameters. LAMOST J1645+4357 has a remarkable abundance set, highlighted by these features: (1) Nitrogen is significantly enhanced ([N/Fe]= +1.4) and the total abundance of C and N is also very high ([(C+N)/Fe]=+0.9);(2) α-elements are over-abundant with respect to iron as generally found in very metal-poor stars;(3) Ti, Sc, Co and Zn are significantly deficient;(4) Cr and Mn are enhanced compared to most of very metal-poor stars;(5) Sr and Ba are deficient and the Sr/Ba ratio ([Sr/Ba]= −1.0) is significantly lower than the value expected for the r-process. The overall abundance pattern of this object from C to Zn is well reproduced by a faint supernova model assuming spherical explosion, except for the excess of Cr and Mn which requires enhancement of incomplete Si burning or small contributions of a type Ia supernova or a pair-instability supernova. There remains, however, a question why the abundance pattern of this star is so unique among very metal-poor stars. Copyright © 2023, The Authors. All rights reserved.

关键词： Supernovae

来源：评论

学校读者我要写书评

暂无评论

Centrality dependence of Lévy-stable two-pion Bose-Einstein correlations in √sNN = 200 GeV Au+Au collisions.

arXiv

引用

arXiv 2024年

作者： Abdulameer, N.J. Acharya, U. Adare, A. Aidala, C. Ajitanand, N.N. Akiba, Y. Akimoto, R. Al-Ta’ani, H. Alexander, J. Angerami, A. Aoki, K. Apadula, N. Aramaki, Y. Asano, H. Aschenauer, E.C. Atomssa, E.T. Awes, T.C. Azmoun, B. Babintsev, V. Bai, M. Bannier, B. Barish, K.N. Bassalleck, B. Bathe, S. Baublis, V. Baumgart, S. Bazilevsky, A. Belmont, R. Berdnikov, A. Berdnikov, Y. Bichon, L. Blankenship, B. Blau, D.S. Bok, J.S. Borisov, V. Boyle, K. Brooks, M.L. Buesching, H. Bumazhnov, V. Butsyk, S. Campbell, S. Castera, P. Chen, C.-H. Chen, D. Chiu, M. Chi, C.Y. Choi, I.J. Choi, J.B. Choi, S. Choudhury, R.K. Christiansen, P. Chujo, T. Chvala, O. Cianciolo, V. Citron, Z. Cole, B.A. Connors, M. Corliss, R. Csanád, M. Csörgo, T. D’Orazio, L. Dairaku, S. Datta, A. Daugherity, M.S. David, G. Denisov, A. Deshpande, A. Desmond, E.J. Dharmawardane, K.V. Dietzsch, O. Ding, L. Dion, A. Donadelli, M. Doomra, V. Drapier, O. Drees, A. Drees, K.A. Durham, J.M. Durum, A. Edwards, S. Efremenko, Y.V. Engelmore, T. Enokizono, A. Esha, R. Eyser, K.O. Fadem, B. Fields, D.E. Finger, M. Finger, M. Firak, D. Fitzgerald, D. Fleuret, F. Fokin, S.L. Frantz, J.E. Franz, A. Frawley, A.D. Fukao, Y. Fusayasu, T. Gainey, K. Gal, C. Garishvili, A. Garishvili, I. Glenn, A. Gong, X. Gonin, M. Goto, Y. de Cassagnac, R. Granier Grau, N. Greene, S.V. Perdekamp, M. Grosse Gunji, T. Guo, L. Guo, T. Gustafsson, H.-Å. Hachiya, T. Haggerty, J.S. Hahn, K.I. Hamagaki, H. Hanks, J. Hashimoto, K. Haslum, E. Hayano, R. Hemmick, T.K. Hester, T. He, X. Hill, J.C. Hodges, A. Hollis, R.S. Homma, K. Hong, B. Horaguchi, T. Hori, Y. Ichihara, T. Iinuma, H. Ikeda, Y. Imrek, J. Inaba, M. Iordanova, A. Isenhower, D. Issah, M. Ivanishchev, D. Jacak, B.V. Javani, M. Jiang, X. Ji, Z. Johnson, B.M. Joo, K.S. Jouan, D. Jumper, D.S. Kamin, J. Kaneti, S. Kang, B.H. Kang, J.H. Kang, J.S. Kapustinsky, J. Karatsu, K. Kasai, M. Abilene Christian University AbileneTX79699 United States Department of Physics Augustana University Sioux FallsSD57197 United States Department of Physics Banaras Hindu University Varanasi221005 India Bhabha Atomic Research Centre Bombay400 085 India Baruch College City University of New York New YorkNY10010 United States Collider-Accelerator Department Brookhaven National Laboratory UptonNY11973-5000 United States Physics Department Brookhaven National Laboratory UptonNY11973-5000 United States University of California-Riverside RiversideCA92521 United States Charles University Faculty of Mathematics and Physics Troja Prague180 00 Czech Republic Center for Nuclear Study Graduate School of Science University of Tokyo 7-3-1 Hongo Tokyo Bunkyo113-0033 Japan University of Colorado BoulderCO80309 United States Columbia University New YorkNY10027 United States Nevis Laboratories IrvingtonNY10533 United States Czech Technical University Zikova 4 Prague 6166 36 Czech Republic Dapnia CEA Saclay Gif-sur-YvetteF-91191 France Debrecen University Egyetem tér 1 DebrecenH-4010 Hungary ELTE Eötvös Loránd University Pázmány P. s. 1/A BudapestH-1117 Hungary Ewha Womans University Seoul120-750 Korea Republic of Florida State University TallahasseeFL32306 United States Georgia State University AtlantaGA30303 United States Hanyang University Seoul133-792 Korea Republic of Hiroshima University Hiroshima Higashi-Hiroshima739-8526 Japan HUN-REN ATOMKI Bem tér 18/c DebrecenH-4026 Hungary IHEP Protvino State Research Center of Russian Federation Institute for High Energy Physics Protvino142281 Russia University of Illinois at Urbana-Champaign UrbanaIL61801 United States Institute for Nuclear Research of the Russian Academy of Sciences prospekt 60-letiya Oktyabrya 7a Moscow117312 Russia Institute of Physics Academy of Sciences of the Czech Republic Na Slovance 2 Prague 8182 21 Czech Republic Iowa State University Ames

The PHENIX experiment measured the centrality dependence of two-pion Bose-Einstein correlation functions in √sNN = 200 GeV Au+Au collisions at the Relativistic Heavy Ion Collider at Brookhaven National Laboratory. The data are well represented by Lévy-stable source distributions. The extracted source parameters are the correlation-strength parameter λ, the Lévy index of stability α, and the Lévy-scale parameter R as a function of transverse mass mT and centrality. The λ(mT) parameter is constant at larger values of mT, but decreases as mT decreases. The Lévy scale parameter R(mT) decreases with mT and exhibits proportionality to the length scale of the nuclear overlap region. The Lévy exponent α(mT) is independent of mT within uncertainties in each investigated centrality bin, but shows a clear centrality dependence. At all centralities, the Lévy exponent α is significantly different from that of Gaussian (α = 2) or Cauchy (α = 1) source distributions. Comparisons to the predictions of Monte-Carlo simulations of resonance-decay chains show that in all but the most-peripheral centrality class (50%–60%), the obtained results are inconsistent with the measurements, unless a significant reduction of the in-medium mass of the η′ meson is included. In each centrality class, the best value of the in-medium η′ mass is compared to the mass of the η meson, as well as to several theoretical predictions that consider restoration of UA(1) symmetry in hot hadronic matter. Copyright © 2024, The Authors. All rights reserved.

关键词： Heavy ions

来源：评论

学校读者我要写书评

暂无评论

Limits on astrophysical antineutrinos with the KamLAND experiment

arXiv

引用

arXiv 2021年

作者： Abe, S. Asami, S. Gando, A. Gando, Y. Gima, T. Goto, A. Hachiya, T. Hata, K. Hayashida, S. Hosokawa, K. Ichimura, K. Ieki, S. Ikeda, H. Inoue, K. Ishidoshiro, K. Kamei, Y. Kawada, N. Kishimoto, Y. Kinoshita, T. Koga, M. Maemura, N. Mitsui, T. Miyake, H. Nakamura, K. Nakamura, K. Nakamura, R. Ozaki, H. Sakai, T. Sambonsugi, H. Shimizu, I. Shirahata, Y. Shirai, J. Shiraishi, K. Suzuki, A. Suzuki, Y. Takeuchi, A. Tamae, K. Ueshima, K. Wada, Y. Watanabe, H. Yoshida, Y. Obara, Shuhei Ichikawa, A.K. Kozlov, A. Chernyak, D. Takemoto, Y. Yoshida, S. Umehara, S. Fushimi, K. Hirata, S. Nakamura, K.Z. Yoshida, M. Berger, B.E. Fujikawa, B.K. Learned, J.G. Maricic, J. Axani, S.N. Winslow, L.A. Fu, Z. Ouellet, J. Efremenko, Y. Karwowski, H.J. Markoff, D.M. Tornow, W. Li, A. Detwiler, J.A. Enomoto, S. Decowski, M.P. Grant, C. Dell’Oro, S. O’Donnell, T. Research Center for Neutrino Science Tohoku University Sendai980-8578 Japan Institute for the Physics and Mathematics of the Universe The University of Tokyo Kashiwa277-8568 Japan Graduate Program on Physics for the Universe Tohoku University Sendai980-8578 Japan Frontier Research Institute for Interdisciplinary Sciences Tohoku University Sendai980-8578 Japan Department of Physics Tohoku University Sendai980-8578 Japan Osaka University Ibaraki Osaka567-0047 Japan Graduate School of Science Osaka University Toyonaka Osaka560-0043 Japan Graduate School of Advanced Technology and Science Tokushima University Tokushima770-8506 Japan Graduate School of Integrated Arts and Sciences Tokushima University Tokushima770-8502 Japan Department of Physics Kyoto University Kyoto606-8502 Japan Nuclear Science Division Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Department of Physics and Astronomy University of Hawaii at Manoa HonoluluHI96822 United States Massachusetts Institute of Technology CambridgeMA02139 United States Department of Physics and Astronomy University of Tennessee KnoxvilleTN37996 United States Triangle Universities Nuclear Laboratory DurhamNC27708 United States University of North Carolina at Chapel Hill Chapel HillNC27599 United States North Carolina Central University DurhamNC27701 United States Physics Department at Duke University DurhamNC27705 United States Center for Experimental Nuclear Physics and Astrophysics University of Washington SeattleWA98195 United States Nikhef University of Amsterdam Science Park Amsterdam Netherlands Boston University BostonMA02215 United States Center for Neutrino Physics Virginia Polytechnic Institute and State University BlacksburgVA24061 United States

We report on a search for electron antineutrinos (¯ νe) from astrophysical sources in the neutrino energy range 8.3 to 30.8 MeV with the KamLAND detector. In an exposure of 6.72 kton-year of the liquid scintillator, we observe 18 candidate events via the inverse beta decay reaction. Although there is a large background uncertainty from neutral current atmospheric neutrino interactions, we find no significant excess over background model predictions. Assuming several supernova relic neutrino spectra, we give upper flux limits of 60–110 cm−2s−1 (90% CL) in the analysis range and present a model-independent flux. We also set limits on the annihilation rates for light dark matter pairs to neutrino pairs. These data improves on the upper probability limit of 8B solar neutrinos converting into ν¯e’s, Pνe→ν¯e −5 (90% CL) assuming an undistorted ν¯e shape. This corresponds to a solar ν¯e flux of 60 cm−2s−1 (90% CL) in the analysis energy range. © 2021, CC BY-NC-ND.

关键词： Galaxies

来源：评论

学校读者我要写书评

暂无评论

建议与咨询留下您的常用邮箱和电话号码，以便我们向您反馈解决方案和替代方法

时间限定

文献类型

馆藏选择

核心期刊

语言

文献类型

帮助

文字说明：

检索规则说明：

检索范例：

分类表

所选分类

限定检索结果

文献类型

馆藏范围

日期分布

学科分类号

主题

机构

作者

语言

请选择保存的检索档案：

请选择收藏分类：

通借通还

建议与咨询 留下您的常用邮箱和电话号码，以便我们向您反馈解决方案和替代方法

时间限定

文献类型

馆藏选择

核心期刊

语言

文献类型

帮助

文字说明：

检索规则说明：

检索范例：

分类表

所选分类

限定检索结果

文献类型

馆藏范围

日期分布

学科分类号

主题

机构

作者

语言

请选择保存的检索档案： 新增检索档案 确定 取消

请选择收藏分类： 新增自定义分类 确定 取消

通借通还

建议与咨询留下您的常用邮箱和电话号码，以便我们向您反馈解决方案和替代方法

请选择保存的检索档案：

请选择收藏分类：