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arXiv 2023年

作者： Zhou, Dengke Wang, Pei Li, Di Fang, Jianhua Miao, Chenchen Freire, Paulo C.C. Zhang, Lei Zhang, Dandan Chen, Huaxi Feng, Yi Xiao, Yifan Xie, Jintao Zhang, Xu Jin, Chenwu Wang, Han Ke, Yinan Guo, Xuerong Zhao, Rushuang Niu, Chenhui Zhu, Weiwei Xue, Mengyao Wang, Yabiao Wu, Jiafu Gan, Zhenye Sun, Zhongyi Wang, Chengjie Zhang, Junshuo Cao, Jinhuang Lu, Wanjin Zhang, Jie Research Center for Astronomical Computing Zhejiang Laboratory Hangzhou311121 China National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China Institute for Frontiers in Astronomy and Astrophysics Beijing Normal University Beijing102206 China University of Chinese Academy of Sciences Beijing100049 China New Cornerstone Science Laboratory Shenzhen518054 China Max Planck Institut für Radioastronomie Bonn53121 Germany Centre for Astrophysics and Supercomputing Swinburne University of Technology Hawthorn3122 Australia School of Mathematical Sciences School of Physics and Electronic Sciences Guizhou Normal University Guiyang550001 China Guizhou Provincial Key Laboratory of Radio Astronomy and Data Processing Guiyang550001 China School of Physics and Electronic Engineering Qilu Normal University Jinan250200 China School of Physics and Electronic Science Guizhou Normal University Guiyang550001 China College of Physical Science and Technology Central China Normal University Wuhan430079 China Tencent Youtu Lab Shanghai201103 China

Globular clusters harbor numerous millisecond pulsars, but long-period pulsars (P 100 ms) are rarely found. In this study, we employed a fast folding algorithm to analyze observational data from multiple globular clusters obtained by the Five-hundred-meter Aperture Spherical radio Telescope (FAST), aiming to detect the existence of long-period pulsars. We estimated the impact of the median filtering algorithm in eliminating red noise on the minimum detectable flux density (Smin) of pulsars. Subsequently, we successfully discovered two isolated long-period pulsars in M15 with periods approximately equal to 1.928451 seconds and 3.960716 seconds, respectively. On the P − P diagram, both pulsars are positioned below the spin-up line, suggesting a possible history of partial recycling in X-ray binary systems disrupted by dynamical encounters later on. According to timing results, these two pulsars exhibit remarkably strong magnetic fields. If the magnetic fields were weakened during the accretion process, then a short duration of accretion might explain the strong magnetic fields of these pulsars. © 2023, CC BY.

关键词： Magnetic fields

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Analytical Rayleigh potential for the general relativistic Poynting-Robertson effect

arXiv

引用

arXiv 2019年

作者： de Falco, Vittorio Battista, Emmanuele Research Centre for Computational Physics and Data Processing Faculty of Philosophy & Science Silesian University in Opava Bezručovo nám. 13 OpavaCZ-746 01 Czech Republic

–We determine the analytic expression of the Rayleigh potential associated to the general relativistic Poynting-Robertson effect. This constitutes the first example of a physical dissipative system treated analytically in General Relativity. The employed approach and further implications are discussed. Copyright © 2019, The Authors. All rights reserved.

关键词： Relativity

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Automatic Diagnosis of Myocarditis Disease in Cardiac MRI Modality using Deep Transformers and Explainable Artificial Intelligence

arXiv

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arXiv 2022年

作者： Jafari, Mahboobeh Shoeibi, Afshin Ghassemi, Navid Heras, Jonathan Ling, Sai Ho Beheshti, Amin Zhang, Yu-Dong Wang, Shui-Hua Alizadehsani, Roohallah Gorriz, Juan M. Acharya, U. Rajendra Rokny, Hamid Alinejad 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 Department of Mathematics and Computer Science University of La Rioja La Rioja Spain Australia Data Analytics Lab Department of Computing Macquarie University SydneyNSW2109 Australia School of Computing and Mathematical Sciences University of Leicester Leicester United Kingdom Deakin University VIC3217 Australia Department of Psychiatry University of Cambridge United Kingdom School of Mathematics Physics and Computing University of Southern Queensland Springfield Australia 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 Research Centre Macquarie University Sydney2109 Australia

Myocarditis is a significant cardiovascular disease (CVD) that poses a threat to the health of many individuals by causing damage to the myocardium. The occurrence of microbes and viruses, including the likes of HIV, plays a crucial role in the development of myocarditis disease (MCD). The images produced during cardiac magnetic resonance imaging (CMRI) scans are low contrast, which can make it challenging to diagnose cardiovascular diseases. In other hand, checking numerous CMRI slices for each CVD patient can be a challenging task for medical doctors. To overcome the existing challenges, researchers have suggested the use of artificial intelligence (AI)-based computer-aided diagnosis systems (CADS). The presented paper outlines a CADS for the detection of MCD from CMR images, utilizing deep learning (DL) methods. The proposed CADS consists of several steps, including dataset, preprocessing, feature extraction, classification, and post-processing. First, the Z-Alizadeh dataset was selected for the experiments. Subsequently, the CMR images underwent various preprocessing steps, including denoising, resizing, as well as data augmentation (DA) via CutMix and MixUp techniques. In the following, the most current deep pre-trained and transformer models are used for feature extraction and classification on the CMR images. The findings of our study reveal that transformer models exhibit superior performance in detecting MCD as opposed to pre-trained architectures. In terms of DL architectures, the Turbulence Neural Transformer (TNT) model exhibited impressive accuracy, reaching 99.73% utilizing a 10-fold cross-validation approach. Additionally, to pinpoint areas of suspicion for MCD in CMRI images, the Explainable-based Grad Cam method was employed. © 2022, CC BY-NC-ND.

关键词： Diseases

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21-cm Signal from the Epoch of Reionization: A Machine Learning upgrade to Foreground Removal with Gaussian Process Regression

arXiv

引用

arXiv 2023年

作者： Acharya, Anshuman Mertens, Florent Ciardi, Benedetta Ghara, Raghunath Koopmans, Léon V.E. Giri, Sambit K. Hothi, Ian Ma, Qing-Bo Mellema, Garrelt Munshi, Satyapan Max-Planck-Institut für Astrophysik Garching85748 Germany LERMA Observatoire de Paris PSL Research University CNRS Sorbonne Université ParisF-75014 France Astrophysics Research Centre Open University of Israel Ra'anana4353701 Israel Kapteyn Astronomical Institute University of Groningen P.O. Box 800 Groningen9700AV Netherlands Nordita KTH Royal Institute of Technology and Stockholm University Hannes Alfvéns väg 12 StockholmSE-106 91 Sweden Laboratoire de Physique de l'ENS ENS Université PSL CNRS Sorbonne Université Universitée Paris Cité Paris75005 France School of Physics and Electronic Science Guizhou Normal University Guiyang550001 China Guizhou Provincial Key Laboratory of Radio Astronomy and Data Processing Guizhou Normal University Guiyang550001 China The Oskar Klein Centre Department of Astronomy Stockholm University AlbaNova StockholmSE-10691 Sweden

In recent years, a Gaussian Process Regression (GPR) based framework has been developed for foreground mitigation from data collected by the LOw-Frequency ARray (LOFAR), to measure the 21-cm signal power spectrum from the Epoch of Reionization (EoR) and Cosmic Dawn. However, it has been noted that through this method there can be a significant amount of signal loss if the EoR signal covariance is misestimated. To obtain better covariance models,we propose to use a kernel trained on the GRIZZLY simulations using a Variational Auto-Encoder (VAE) based algorithm. In this work, we explore the abilities of this Machine Learning based kernel (VAE kernel) used with GPR, by testing it on mock signals from a variety of simulations, exploring noise levels corresponding to ≈10 nights (≈141 hours) and ≈100 nights (≈1410 hours) of observations with LOFAR. Our work suggests the possibility of successful extraction of the 21-cm signal within 2σ uncertainty in most cases using the VAE kernel, with better recovery of both shape and power than with previously used covariance models. We also explore the role of the excess noise component identified in past applications of GPR and additionally analyse the possibility of redshift dependence on the performance of the VAE kernel. The latter allows us to prepare for future LOFAR observations at a range of redshifts, as well as compare with results from other telescopes. © 2023, CC BY.

关键词： Cosmology

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Habitable zones around almost extremely spinning black holes (black sun revisited)

arXiv

引用

arXiv 2020年

作者： Bakala, Pavel Dočekal, Jan Turoňová, Zuzana Research Centre for Computational Physics and Data Processing Faculty of Philosophy and Science Bezrucovonam. 13 OpavaCZ-746 01 Czech Republic M. R. Stefánik Observatory and Planetarium Sládkovicova 41 Hlohovec920 01 Slovakia INAF - Osservatorio Astronomico di Roma Via Frascati 33 Monteporzio Catone Roma00078 Italy

We analyzed the thermodynamics of hypothetical exoplanets at very low Keplerian circular orbits in close vicinity of rapidly spinning supermassive black holes. Such black hole exoplanets are heated by strongly blueshifted and focused flux of the incoming cosmic microwave background (CMB) and cooled by the cold part of the local sky containing the black hole shadow. This gives rise to a temperature difference, which can drive processes far from thermodynamic equilibrium in a hypothetical life form inhabiting black hole exoplanets, similar to the case of a planet heated by the radiation of the parent star and cooled by the night sky. We found that for a narrow range of radii of very low Keplerian circular orbits and for very high spin of a supermassive black hole, the temperature regime of the black hole exoplanets corresponds to the habitable zone around standard stars. The thermodynamics of black hole exoplanets therefore, in principle, does not exclude the existence of life based on known biology. The peak of the multiblackbody spectral profile of the CMB heating the exoplanet is located in the ultraviolet band, but a significant fraction of the flux comes also in the visible and infrared bands. The minimum mass of a black hole ensuring the resistance to tidal disruption of an Earth-like exoplanet orbiting in the habitable zone is estimated to 1.63 108mo. Copyright © 2020, The Authors. All rights reserved.

关键词： Extrasolar planets

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Physical Publicly Verifiable Randomness from Pulsars

arXiv

引用

arXiv 2022年

作者： Dawson, Joanne R. Hobbs, George Gao, Yansong Camtepe, Seyit Pieprzyk, Josef Feng, Yi Tranfa, Luke Bradbury, Sarah Zhu, Weiwei Li, Di CSIRO Space and Astronomy Australia Telescope National Facility PO Box 76 EppingNSW1710 Australia Department of Physics and Astronomy MQ Research Centre in Astronomy Astrophysics and Astrophotonics Macquarie University NSW2109 Australia School of Computer Science and Engineering Nanjing University of Science and Technology Nanjing210094 China CSIRO Data61 PO Box 76 EppingNSW1710 Australia Institute of Computer Science Polish Academy of Sciences Poland National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China University of Chinese Academy of Sciences Beijing100049 China BrisbaneQLD4001 Australia NAOC-UKZN Computational Astrophysics Centre University of KwaZulu-Natal Durban4000 South Africa

We demonstrate how radio pulsars can be used as random number generators. Specifically, we focus on publicly verifiable randomness (PVR), in which the same sequence of trusted and verifiable random numbers is obtained by multiple parties. PVR is a critical building block for many processes and algorithms (including cryptography, scientific trials, electoral audits and international treaties). However, current approaches (based on number theory) may soon become vulnerable to quantum computers, motivating a growing demand for PVR based on natural physical phenomena. In this context, we explore pulsars as a potential physical PVR source. We first show that bit sequences extracted from the measured flux densities of a bright millisecond pulsar can pass standardised tests for randomness. We then quantify three illustrative methods of bit-extraction from pulsar flux density sequences, using simultaneous observations of a second pulsar carried out with the Parkes telescope in Australia and the Five-hundred-metre Aperture Spherical radio Telescope (FAST) in China, supported by numerical simulations. We demonstrate that the same bit sequence can indeed be obtained at both observatories, but the ubiquitous presence of radiometer noise needs to be accounted for when determining the expected bit error rate between two independent sequences. We discuss our results in the context of an imaginary use-case in which two mutually distrusting parties wish to obtain the same random bit sequence, exploring potential methods to mitigate against a malicious participant. © 2022, CC BY-NC-ND.

关键词： Random processes

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Three-dimensional general relativistic Poynting-Robertson effect. III. Static and non-spherical quadrupolar massive source

arXiv

引用

arXiv 2020年

作者： de Falco, Vittorio Bakala, Pavel Falanga, Maurizio M. R. Štefánik Observatory Planetarium Sládkovičova 41 Hlohovec920 01 Slovakia Research Centre for Computational Physics and Data Processing Faculty of Philosophy & Science Silesian University in Opava Bezručovo nám. 13 OpavaCZ-74601 Czech Republic International Space Science Institute Hallerstrasse 6 Bern3012 Switzerland

We investigate the three-dimensional (3D) motion of a test particle in the gravitational field generated by a non-spherical compact object endowed with a mass quadrupole moment, described by the Erez-Rosen metric, and a radiation field, including the general relativistic Poynting-Robertson (PR) effect, coming from a rigidly rotating spherical emitting source located outside of the compact object. We derive the equations of motion for test particles influenced by such radiation field, recovering the two-dimensional (2D) description, and the weak-field approximation. This dynamical system admits the existence of a critical hypersurface, region where gravitational and radiation forces balance. Selected test particle orbits for different set of input parameters are displayed. The possible configurations on the critical hypersurfaces can be either latitudinal drift towards the equatorial ring or suspended orbits. We discuss about the existence of multiple hypersurface solutions through a simple method to perform the calculations. We graphically prove also that the critical hypersurfaces are stable configurations within the Lyapunov theory. Copyright © 2020, The Authors. All rights reserved.

关键词： Dynamical systems

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Beyond UVJ: Color Selection of Galaxies in the JWST Era

arXiv

引用

arXiv 2022年

作者： Antwi-Danso, Jacqueline Papovich, Casey Leja, Joel Marchesini, Danilo Marsan, Z. Cemile Martis, Nicholas S. Labbé, Ivo Muzzin, Adam Glazebrook, Karl Straatman, Caroline M.S. Tran, Kim-Vy H. George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy Texas A&m University College StationTX United States Department of Physics and Astronomy Texas A&m University 4242 TAMU College StationTX United States Department of Astronomy & Astrophysics The Pennsylvania State University University ParkPA16802 United States Institute for Computational & Data Sciences The Pennsylvania State University University ParkPA United States Institute for Gravitation and the Cosmos The Pennsylvania State University University ParkPA16802 United States Department of Physics and Astronomy Tufts University MedfordMA United States Department of Physics and Astronomy York University TorontoON Canada Department of Astronomy and Physics St. Mary's University HalifaxNS Canada National Research Council of Canada Herzberg Astronomy & Astrophysics Research Centre 5071 West Saanich Road VictoriaBCV9E 2E7 Canada Center for Astrophysics & Supercomputing Swinburne University HawthornVIC Australia Department of Physics and Astronomy Ghent University Krijgslaan 281 S9 GentB-9000 Belgium Max-Planck Institut für Astronomie Königstuhl 17 HeidelbergD-69117 Germany School of Physics University of New South Wales Kensington Australia Arc Centre for Excellence in All-Sky Astrophysics in 3D Australia

We present a new rest-frame color-color selection method using "synthetic us- gsand gs- is", (ugi)scolors to identify star-forming and quiescent galaxies. Our method is similar to the widely-used U - V versus V - J (UVJ) diagram. However, UVJ suffers known systematics. Spectroscopic campaigns have shown that UVJ-selected quiescent samples at z 3 include ∼ 10 - 30% contamination from galaxies with dust-obscured star formation and strong emission lines. Moreover, at z > 3, UV J colors are extrapolated because the rest-frame J-band shifts beyond the coverage of the deepest bandpasses at soffers improvements to UVJ at z > 3, and can be applied to galaxies in the JWST era. We apply (ugi)sselection to galaxies at 0.5 0color by up to 1 magnitude, but changes (gs- is)0color by ≤ 0.2 mag, even at z ≅ 6. While (ugi)s-selected quiescent samples are comparable to UV J in completeness (both achieve ∼85-90% at z = 3-3.5), (ugi)sreduces contamination in quiescent samples by nearly a factor of two, from ≅35% to ≅17% at z = 3, and from ≅60% to ≅33% at z = 6. This leads to improvements in the true-to-false-positive ratio (TP/FP), where we find TP/FP 2.2 for (ugi)sat z ≅ 3.5 - 6, compared to TP/FP swill provide higher-fidelity samples. © 2022, CC BY.

关键词： Galaxies

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Deeper multi-redshift upper limits on the Epoch of Reionization 21-cm signal power spectrum from LOFAR between z=8.3 and z=10.1

arXiv

引用

arXiv 2025年

作者： Mertens, F.G. Mevius, M. Koopmans, L.V.E. Offringa, A.R. Zaroubi, S. Acharya, A. Brackenhoff, S.A. Ceccotti, E. Chapman, E. Chege, K. Ciardi, B. Ghara, R. Ghosh, S. Giri, S.K. Hothi, I. Höfer, C. Iliev, I.T. Jelić, V. Ma, Q. Mellema, G. Munshi, S. Pandey, V.N. Yatawatta, S. LUX Observatoire de Paris PSL Research University CNRS Sorbonne Université ParisF-75014 France Astron PO Box 2 Dwingeloo7990 AA Netherlands Kapteyn Astronomical Institute University of Groningen PO Box 800 Groningen9700 AV Netherlands Department of Natural Sciences The Open University of Israel 1 University Road PO Box 808 Ra’anana4353701 Israel Max-Planck Institute for Astrophysics Karl-Schwarzschild-Straße 1 Garching85748 Germany INAF – Istituto di Radioastronomia Via P. Gobetti 101 Bologna40129 Italy School of Physics and Astronomy The University of Nottingham University Park NottinghamNG7 2RD United Kingdom Department of Physical Sciences Indian Institute of Science Education and Research Kolkata WB Mohanpur741 246 India Van Swinderen Institute for Particle Physics and Gravity University of Groningen Nijenborgh 4 Groningen9747 AG Netherlands Nordita KTH Royal Institute of Technology Stockholm University Hannes Alfvéns väg 12 StockholmSE-106 91 Sweden Laboratoire de Physique de l’Ecole Normale Supérieure ENS Université PSL CNRS Sorbonne Université Université de Paris ParisF-75005 France Astronomy Centre Department of Physics and Astronomy Pevensey II Building University of Sussex BrightonBN1 9QH United Kingdom Ruđer Bošković Institute Bijenička cesta 54 Zagreb10000 Croatia School of Physics and Electronic Science Guizhou Normal University Guiyang550001 China Guizhou Provincial Key Laboratory of Radio Astronomy and Data Processing Guizhou Normal University Guiyang550001 China The Oskar Klein Centre Department of Astronomy Stockholm University AlbaNova StockholmSE-10691 Sweden

We present new upper limits on the 21-cm signal power spectrum from the Epoch of Reionization (EoR), at redshifts z ≈ 10.1, 9.1, and 8.3, based on reprocessed observations from the Low-Frequency Array (LOFAR). The analysis incorporates significant enhancements in calibration methods, sky model subtraction, radio-frequency interference (RFI) mitigation, and an improved signal separation technique using machine learning to develop a physically motivated covariance model for the 21-cm signal. These advancements have markedly reduced previously observed excess power due to residual systematics, bringing the measurements closer to the theoretical thermal noise limit across the entire k-space. Using comparable observational data, we achieve a 2 to 4-fold improvement over our previous LOFAR limits, with best upper limits of Δ221 2 at k = 0.076 ℎ cMpc−1, Δ221 2 at k = 0.076 ℎ cMpc−1 and Δ221 2 at k = 0.083 ℎ cMpc−1 at redshifts z ≈ 10.1, 9.1, and 8.3, respectively. These new multi-redshift upper limits provide new constraints that can be used to refine our understanding of the astrophysical processes during the EoR. Comprehensive validation tests, including signal injection, were performed to ensure the robustness of our methods. The remaining excess power is attributed to residual foreground emissions from distant sources, beam model inaccuracies, and low-level RFI. We discuss ongoing and future improvements to the data processing pipeline aimed at further reducing these residuals, thereby enhancing the sensitivity of LOFAR observations in the quest to detect the 21-cm signal from the EoR. © 2025, CC BY.

关键词： Cosmology

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Is fixed-node diffusion quantum Monte Carlo reproducible?

arXiv

引用

arXiv 2025年

作者： Pia, Flaviano Della Shi, Benjamin X. Al-Hamdani, Yasmine S. Alfè, Dario Anderson, Tyler A. Barborini, Matteo Benali, Anouar Casula, Michele Drummond, Neil Dubecký, Matúš Filippi, Claudia Kent, Paul R.C. Krogel, Jaron T. Ríos, Pablo López Lüchow, Arne Luo, Ye Michaelides, Angelos Mitas, Lubos Nakano, Kousuke Needs, Richard Per, Manolo C. Scemama, Anthony Schultze, Jil Shinde, Ravindra Slootman, Emiel Sorella, Sandro Tkatchenko, Alexandre Towler, Mike Umrigar, C.J. Wagner, Lucas K. Wheeler, William A. Zhou, Haihan Zen, Andrea Yusuf Hamied Department of Chemistry University of Cambridge CambridgeCB2 1EW United Kingdom Department of Earth Sciences University College London LondonWC1E 6BT United Kingdom Dipartimento di Fisica Ettore Pancini Università di Napoli Federico II Monte S. Angelo NapoliI-80126 Italy Laboratory of Atomic and Solid State Physics Cornell University IthacaNY14853 United States HPC Platform University of Luxembourg Esch-sur-AlzetteL-4365 Luxembourg Computational Science Division Argonne National Laboratory LemontIL United States Sorbonne Université CNRS UMR 7590 MNHN 4 Place Jussieu Paris75252 France Department of Physics Lancaster University LancasterLA1 4YB United Kingdom Department of Physics Faculty of Science University of Ostrava 30. Dubna 22 Ostrava701 03 Czech Republic MESA+ Institute for Nanotechnology University of Twente Enschede7500 AE Netherlands Computational Sciences and Engineering Division Oak Ridge National Laboratory Oak RidgeTN37831 United States Materials Science and Technology Division Oak Ridge National Laboratory Oak RidgeTN37831 United States Max Planck Institute for Solid State Research Heisenbergstr. 1 Stuttgart70569 Germany Institute of Physical Chemistry RWTH Aachen University Landoltweg 2 Aachen52074 Germany Department of Physics North Carolina State University RaleighNC27695-8202 United States 1-2-1 Sengen Tsukuba Ibaraki305-0047 Japan Theory of Condensed Matter Group Cavendish Laboratory J. J. Thomson Avenue CambridgeCB3 0HE United Kingdom CSIRO Data61 ClaytonVIC3168 Australia Université de Toulouse CNRS UPS Toulouse31062 France International School for Advanced Studies SISSA Trieste34136 Italy Department of Physics and Materials Science University of Luxembourg Luxembourg CityL-1511 Luxembourg The Apuan Alps Centre for Physics Vallico Sotto Italy Department of Physics University of Illinois at Urbana-Champaign UrbanaIL61801 United States Department of Materials Science and Engi

Fixed-node diffusion quantum Monte Carlo (FN-DMC) is a widely-trusted manybody method for solving the Schrödinger equation, known for its reliable predictions of material and molecular properties. Furthermore, its excellent scalabilitywith system complexity and near-perfect utilization of computational power makes FN-DMC ideally positioned to leverage new advances in computing to address increasingly complex scientific problems. Even though the method is widely used as a computational gold standard, reproducibility across the numerous FN-DMC code implementations has yet to be demonstrated. This difficulty stems from the diverse array of DMC algorithms and trial wave functions, compounded by the method's inherent stochastic nature. This study represents a community-wide effort to address the titular question, affirming that: Yes, FN-DMC is reproducible (when handled with care). Using the water-methane dimer as the canonical test case, we compare results from eleven different FN-DMC codes and show that the approximations to treat the non-locality of pseudopotentials are the primary source of the discrepancies between them. In particular, we demonstrate that, for the same choice of determinantal component in the trial wave function, reliable and reproducible predictions can be achieved by employing the T-move (TM), the determinant locality approximation (DLA), or the determinant T-move (DTM) schemes, while the older locality approximation (LA) leads to considerable variability in results. This work lays the foundation to establish accurate and reproducible FN-DMC estimates for all future studies across applications in materials science, physics, chemistry, and biology. © 2025, CC BY.

关键词： Wave functions

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