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arXiv 2024年

作者： Lammers, Caleb Cranmer, Miles Hadden, Sam Ho, Shirley Murray, Norman Tamayo, Daniel Department of Astrophysical Sciences Princeton University 4 Ivy Lane PrincetonNJ08544 United States Department of Applied Mathematics and Theoretical Physics University of Cambridge Wilberforce Road CambridgeCB3 0WA United Kingdom Institute of Astronomy University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom Kavli Institute for Cosmology University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom Canadian Institute for Theoretical Astrophysics University of Toronto 60 St. George Street TorontoONM5S 3H8 Canada Center for Computational Astrophysics Flatiron Institute New YorkNY10010 United States Department of Physics Center for Data Science New York University 726 Broadway New YorkNY10003 United States Department of Physics University of Toronto 60 St. George Street TorontoONM5S 1A7 Canada Department of Physics Harvey Mudd College ClaremontCA91711 United States

Constraining planet formation models based on the observed exoplanet population requires generating large samples of synthetic planetary systems, which can be computationally prohibitive. A significant bottleneck is simulating the giant impact phase, during which planetary embryos evolve gravitationally and combine to form planets, which may themselves experience later collisions. To accelerate giant impact simulations, we present a machine learning (ML) approach to predicting collisional outcomes in multiplanet systems. Trained on more than 500,000 N-body simulations of three-planet systems, we develop an ML model that can accurately predict which two planets will experience a collision, along with the state of the post-collision planets, from a short integration of the system's initial conditions. Our model greatly improves on non-ML baselines that rely on metrics from dynamics theory, which struggle to accurately predict which pair of planets will experience a collision. By combining with a model for predicting long-term stability, we create an ML-based giant impact emulator, which can predict the outcomes of giant impact simulations with reasonable accuracy and a speedup of up to four orders of magnitude. We expect our model to enable analyses that would not otherwise be computationally feasible. As such, we release our training code, along with an easy-to-use API for our collision outcome model and giant impact emulator. Copyright © 2024, The Authors. All rights reserved.

关键词： Exoplanets

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Color superconductivity in a self-consistent NJL-type model

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Physical Review D 2020年第5期102卷 054028-054028页

作者： Li-Qun Su Chao Shi Yong-Hui Xia Hongshi Zong Department of Physics Nanjing University Nanjing 210093 China Department of Nuclear Science and Technology Nanjing University of Aeronautics and Astronautics Nanjing 210016 China Department of Physics Anhui Normal University Wuhu 241000 China Nanjing Proton Source Research and Design Center Nanjing 210093 China Joint Center for Particle Nuclear Physics and Cosmology Nanjing 210093 China

In this paper, the NJL-type model is used to investigate the color superconductivity. The four-fermion interactions of the NJL-type model are Fierz-transformed into two different classes, i.e., the quark-antiquark and the quark-quark interaction channels, associated with the chiral symmetry breaking and color superconductivity respectively. We conclude that the weighting factor between quark-antiquark and quark-quark interaction channels has significance on the phase structure when the mean-field approximation is employed, and the baryon number density gives a tight constraint on the weighting factor of quark-antiquark interaction channels. Besides, the susceptibilities show that the color superconducting phase transition is of the second-order and takes place before the chiral crossover transition as quark number density increases. In the end, we study the critical temperatures Tc of the color superconductivity and it agrees with the perturbative result of diquark condensate Δ≈0.57Tc.

关键词： Nonperturbative effects in field theory Nuclear matter QCD phase transitions

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Study of Mass Composition of Cosmic Rays with IceTop and IceCube 37

Study of Mass Composition of Cosmic Rays with IceTop and Ice...

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37th International Cosmic Ray Conference, ICRC 2021

作者： Koundal, Paras Plum, Matthias Saffer, Julian Abbasi, R. Ackermann, M. Adams, J. Aguilar, J.A. Ahlers, M. Ahrens, M. Alispach, C. Alves, A.A. Amin, N.M. An, R. Andeen, K. Anderson, T. Anton, G. Argüelles, C. Ashida, Y. Axani, S. Bai, X. Balagopal, A.V. Barbano, A. Barwick, S.W. Bastian, B. Basu, V. Baur, S. Bay, R. Beatty, J.J. Becker, K.-H. Becker Tjus, J. Bellenghi, C. BenZvi, S. Berley, D. Bernardini, E. Besson, D.Z. Binder, G. Bindig, D. Blaufuss, E. Blot, S. Boddenberg, M. Bontempo, F. Borowka, J. Böser, S. Botner, O. Böttcher, J. Bourbeau, E. Bradascio, F. Braun, J. Bron, S. Brostean-Kaiser, J. Browne, S. Burgman, A. Burley, R.T. Busse, R.S. Campana, M.A. Carnie-Bronca, E.G. Chen, C. Chirkin, D. Choi, K. Clark, B.A. Clark, K. Classen, L. Coleman, A. Collin, G.H. Conrad, J.M. Coppin, P. Correa, P. Cowen, D.F. Cross, R. Dappen, C. Dave, P. De Clercq, C. DeLaunay, J.J. Dembinski, H. Deoskar, K. De Ridder, S. Desai, A. Desiati, P. de Vries, K.D. de Wasseige, G. de With, M. DeYoung, T. Dharani, S. Diaz, A. Díaz-Vélez, J.C. Dittmer, M. Dujmovic, H. Dunkman, M. DuVernois, M.A. Dvorak, E. Ehrhardt, T. Eller, P. Engel, R. Erpenbeck, H. Evans, J. Evenson, P.A. Fan, K.L. Fazely, A.R. Fiedlschuster, S. Fienberg, A.T. Filimonov, K. Finley, C. Fischer, L. Fox, D. Franckowiak, A. Friedman, E. Fritz, A. Fürst, P. Gaisser, T.K. Gallagher, J. Ganster, E. Garcia, A. Garrappa, S. Gerhardt, L. Ghadimi, A. Glaser, C. Glauch, T. Glüsenkamp, T. Goldschmidt, A. Gonzalez, J.G. Goswami, S. Grant, D. Grégoire, T. Griswold, S. Gündüz, M. Günther, C. Haack, C. Hallgren, A. Halliday, R. Halve, L. Halzen, F. Ha Minh, M. Hanson, K. Hardin, J. Harnisch, A.A. Haungs, A. Hauser, S. Hebecker, D. Helbing, K. Henningsen, F. Hettinger, E.C. Hickford, S. Hignight, J. Hill, C. Hill, G.C. Hoffman, K.D. Hoffmann, R. Hoinka, T. Hokanson-Fasig, B. Hoshina, K. Huang, F. Huber, M. Huber, T. Hultqvist, K. Hünnefeld, M. Hussain, R. Institute for Astroparticle Physics Karlsruhe Institute of Technology Karlsruhe76021 Germany Department of Physics Marquette University MilwaukeeWI53201 United States Institute of Experimental Particle Physics Karlsruhe Institute of Technology Karlsruhe76021 Germany III. Physikalisches Institut RWTH Aachen University AachenD-52056 Germany Department of Physics University of Adelaide Adelaide5005 Australia Dept. of Physics and Astronomy University of Alaska Anchorage 3211 Providence Dr. AnchorageAK99508 United States Dept. of Physics University of Texas at Arlington 502 Yates St. Science Hall Rm 108 Box 19059 ArlingtonTX76019 United States CTSPS Clark-Atlanta University AtlantaGA30314 United States School of Physics Center for Relativistic Astrophysics Georgia Institute of Technology AtlantaGA30332 United States Dept. of Physics Southern University Baton RougeLA70813 United States Dept. of Physics University of California BerkeleyCA94720 United States Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Institut für Physik Humboldt-Universität zu Berlin BerlinD-12489 Germany Fakultät für Physik & Astronomie Ruhr-Universität Bochum BochumD-44780 Germany Université Libre de Bruxelles Science Faculty CP230 BrusselsB-1050 Belgium Dienst ELEM BrusselsB-1050 Belgium Department of Physics Laboratory for Particle Physics and Cosmology Harvard University CambridgeMA02138 United States Dept. of Physics Massachusetts Institute of Technology CambridgeMA02139 United States Dept. of Physics Institute for Global Prominent Research Chiba University Chiba263-8522 Japan Department of Physics Loyola University Chicago ChicagoIL60660 United States Dept. of Physics and Astronomy University of Canterbury Private Bag 4800 Christchurch New Zealand Dept. of Physics University of Maryland College ParkMD20742 United States Dept. of Astronomy Ohio State University ColumbusOH43210 United States Dept. of Physics Cent

The IceCube Neutrino Observatory is a multi-component detector at the South Pole which detects high-energy particles emerging from astrophysical events. These particles provide us with insights into the fundamental properties and behaviour of their sources. Besides its principal usage and merits in neutrino astronomy, using IceCube in conjunction with its surface array, IceTop, also makes it a unique three-dimensional cosmic-ray detector. This distinctive feature helps facilitate detailed cosmic-ray analysis in the transition region from galactic to extragalactic sources. We will present the progress made on multiple fronts to establish a framework for mass-estimation of primary cosmic rays. The first technique relies on a likelihood-based analysis of the surface signal distribution and improves upon the standard reconstruction technique. The second uses advanced methods in graph neural networks to use the full in-ice shower footprint, in addition to global shower-footprint features from IceTop. A comparison between the two methods for composition analysis as well as a possible extension of the analysis techniques for sub-PeV cosmic-ray air-showers will also be discussed. © Copyright owned by the author(s).

关键词： Cosmic rays

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Searching for time-dependent high-energy neutrino emission from X-ray binaries with IceCube 37

Searching for time-dependent high-energy neutrino emission f...

引用

37th International Cosmic Ray Conference, ICRC 2021

作者： Liu, Qinrui Kheirandish, Ali Abbasi, R. Ackermann, M. Adams, J. Aguilar, J.A. Ahlers, M. Ahrens, M. Alispach, C. Alves, A.A. Amin, N.M. An, R. Andeen, K. Anderson, T. Anton, G. Argüelles, C. Ashida, Y. Axani, S. Bai, X. Balagopal, A.V. Barbano, A. Barwick, S.W. Bastian, B. Basu, V. Baur, S. Bay, R. Beatty, J.J. Becker, K.-H. Becker Tjus, J. Bellenghi, C. BenZvi, S. Berley, D. Bernardini, E. Besson, D.Z. Binder, G. Bindig, D. Blaufuss, E. Blot, S. Boddenberg, M. Bontempo, F. Borowka, J. Böser, S. Botner, O. Böttcher, J. Bourbeau, E. Bradascio, F. Braun, J. Bron, S. Brostean-Kaiser, J. Browne, S. Burgman, A. Burley, R.T. Busse, R.S. Campana, M.A. Carnie-Bronca, E.G. Chen, C. Chirkin, D. Choi, K. Clark, B.A. Clark, K. Classen, L. Coleman, A. Collin, G.H. Conrad, J.M. Coppin, P. Correa, P. Cowen, D.F. Cross, R. Dappen, C. Dave, P. De Clercq, C. DeLaunay, J.J. Dembinski, H. Deoskar, K. De Ridder, S. Desai, A. Desiati, P. de Vries, K.D. de Wasseige, G. de With, M. DeYoung, T. Dharani, S. Diaz, A. Díaz-Vélez, J.C. Dittmer, M. Dujmovic, H. Dunkman, M. DuVernois, M.A. Dvorak, E. Ehrhardt, T. Eller, P. Engel, R. Erpenbeck, H. Evans, J. Evenson, P.A. Fan, K.L. Fazely, A.R. Fiedlschuster, S. Fienberg, A.T. Filimonov, K. Finley, C. Fischer, L. Fox, D. Franckowiak, A. Friedman, E. Fritz, A. Fürst, P. Gaisser, T.K. Gallagher, J. Ganster, E. Garcia, A. Garrappa, S. Gerhardt, L. Ghadimi, A. Glaser, C. Glauch, T. Glüsenkamp, T. Goldschmidt, A. Gonzalez, J.G. Goswami, S. Grant, D. Grégoire, T. Griswold, S. Gündüz, M. Günther, C. Haack, C. Hallgren, A. Halliday, R. Halve, L. Halzen, F. Ha Minh, M. Hanson, K. Hardin, J. Harnisch, A.A. Haungs, A. Hauser, S. Hebecker, D. Helbing, K. Henningsen, F. Hettinger, E.C. Hickford, S. Hignight, J. Hill, C. Hill, G.C. Hoffman, K.D. Hoffmann, R. Hoinka, T. Hokanson-Fasig, B. Hoshina, K. Huang, F. Huber, M. Huber, T. Hultqvist, K. Hünnefeld, M. Hussain, R. In, S. Iovine, N. Department of Physics University of Wisconsin-Madison MadisonWI53706 United States Department of Physics Department of Astronomy & Astrophysics Center for Multimessenger Astrophysics Institute for Gravitation & the Cosmos The Pennsylvania State University University ParkPA16802 United States III. Physikalisches Institut RWTH Aachen University AachenD-52056 Germany Department of Physics University of Adelaide Adelaide5005 Australia Dept. of Physics and Astronomy University of Alaska Anchorage 3211 Providence Dr. AnchorageAK99508 United States Dept. of Physics University of Texas at Arlington 502 Yates St. Science Hall Rm 108 Box 19059 ArlingtonTX76019 United States CTSPS Clark-Atlanta University AtlantaGA30314 United States School of Physics Center for Relativistic Astrophysics Georgia Institute of Technology AtlantaGA30332 United States Dept. of Physics Southern University Baton RougeLA70813 United States Dept. of Physics University of California BerkeleyCA94720 United States Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Institut für Physik Humboldt-Universität zu Berlin BerlinD-12489 Germany Fakultät für Physik & Astronomie Ruhr-Universität Bochum BochumD-44780 Germany Université Libre de Bruxelles Science Faculty CP230 BrusselsB-1050 Belgium Dienst ELEM BrusselsB-1050 Belgium Department of Physics Laboratory for Particle Physics and Cosmology Harvard University CambridgeMA02138 United States Dept. of Physics Massachusetts Institute of Technology CambridgeMA02139 United States Dept. of Physics Institute for Global Prominent Research Chiba University Chiba263-8522 Japan Department of Physics Loyola University Chicago ChicagoIL60660 United States Dept. of Physics and Astronomy University of Canterbury Private Bag 4800 Christchurch New Zealand Dept. of Physics University of Maryland College ParkMD20742 United States Dept. of Astronomy Ohio State University ColumbusOH43210 United St

X-ray binaries are long-standing source candidates of Galactic cosmic rays and neutrinos. The compact object in a binary system can be the site for cosmic-ray acceleration, while high-energy neutrinos can be produced by the interactions of cosmic rays in the jet of the compact object, the stellar wind, or the atmosphere of the companion star. We report a time-dependent study of high-energy neutrinos from X-ray binaries with IceCube using 7.5 years of muon neutrino data and X-ray observations. In the absence of significant correlation, we report upper limits on the neutrino fluxes from these sources and provide a comparison with theoretical predictions. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Cosmic rays

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The origin of UV/optical emission in the black hole low-mass X-ray binary Swift J1753.5-0127

arXiv

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arXiv 2022年

作者： Yang, Pengcheng Zhang, Guobao Russell, David M. Gelfand, Joseph D. Méndez, Mariano Wang, Jiancheng Lyu, Ming Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution Celestial Objects Chinese Academy of Sciences Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences Bejing100012 China University of Chinese Academy of Sciences Bejing100049 China New York University Abu Dhabi P.O. Box 129188 Abu Dhabi United Arab Emirates Center for Astro Particle and Planetary Physics New York University Abu Dhabi P.O. Box 129188 Abu Dhabi United Arab Emirates Center for Cosmology and Particle Physics New York University 726 Broadway New YorkNY10003 United States Kapteyn Astronomical Institute University of Groningen P.O. Box 800 NL-9700 AV Groningen Netherlands Department of Physics Xiangtan University Hunan Xiangtan411105 China Key Laboratory of Stars and Interstellar Medium Xiangtan University Hunan Xiangtan411105 China

The emission from the accreting black holes (BHs) in low-mass X-ray binaries (LMXBs) covers a broad energy band from radio to X-rays. Studying the correlations between emission in different energy bands during outbursts can provide valuable information about the accretion process. We analyse the simultaneous optical, ultraviolet (UV) and X-ray data of the BHLMXB Swift J1753.5-0127 during its ∼ 12-year long outburst with the Neil Gehrels Swift Observatory. We find that the UV/optical and X-ray emission are strongly correlated during the hard states of the outburst. We fit the relation with a power-law function FUV/optical∝ FβXand find that the power-law index β increases from ∼ 0.24 to ∼ 0.33 as the UV/optical wavelength decreases from ∼ 5400 Å (V) to ∼ 2030 Å (UVW2). We explore the possible reasons for this and suggest that in Swift J1753.5-0127 the UV/optical emission is dominated by a viscously heated accretion disc at large radii. We find that the data that deviate from the correlation correspond to the low-intensity peaks appeared in the X-ray band during the outburst, and suggest that these deviations are driven by the emission from the inner part of the accretion disc. Copyright © 2022, The Authors. All rights reserved.

关键词： Stars

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Lattice nucleon isovector unpolarized Parton distribution in the physical-continuum limit

arXiv

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arXiv 2020年

作者： Lin, Huey-Wen Chen, Jiunn-Wei Zhang, Rui Department of Physics and Astronomy Michigan State University East LansingMI48824 United States Department of Computational Mathematics Science and Engineering Michigan State University East LansingMI48824 United States Department of Physics Center for Theoretical Physics Leung Center for Cosmology and Particle Astrophysics Taiwan

We present the first lattice-QCD calculation of the nucleon isovector unpolarized parton distribution functions (PDFs) at the physical-continuum limit using Large-Momentum Effective Theory (LaMET). The lattice results are calculated using ensembles with multiple sea pion masses with the lightest one around 135 MeV, 3 lattice spacings a ∈ [0.06, 0.12] fm, and multiple volumes with MπL ranging 3.3 to 5.5. We perform a simultaneous chiral-continuum extrapolation to obtain RI/MOM renormalized nucleon matrix elements with various Wilson-link displacements in the continuum limit at physical pion mass. Then, we apply one-loop perturbative matching to the quasi-PDFs to obtain the lightcone PDFs. We find the lattice-spacing dependence to be much larger than the dependence on pion mass and lattice volume for these LaMET matrix elements. Our physical-continuum limit unpolarized isovector nucleon PDFs are found to be consistent with global-PDF results. Copyright © 2020, The Authors. All rights reserved.

关键词： Hadrons

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Progress Towards a Diffuse Neutrino Search in the Full Livetime of the Askaryan Radio Array

arXiv

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arXiv 2023年

作者： Dasgupta, Paramita Muzio, Marco Stein Ali, S. Allison, P. Archambault, S. Beatty, J.J. Besson, D.Z. Bishop, A. Chen, P. Chen, Y.C. Clark, B.A. Clay, W. Connolly, A. Couberly, K. Cremonesi, L. Cummings, A. Dasgupta, P. Debolt, R. de Kockere, S. de Vries, K.D. Deaconu, C. DuVernois, M.A. Flaherty, J. Friedman, E. Gaior, R. Giri, P. Hanson, J. Harty, N. Hendricks, B. Hoffman, K.D. Huang, J.J. Huang, M.-H. Hughes, K. Ishihara, A. Karle, A. Kelley, J.L. Kim, K.-C. Kim, M.-C. Kravchenko, I. Krebs, R. Kuo, C.Y. Kurusu, K. Latif, U.A. Liu, C.H. Liu, T.C. Luszczak, W. Mase, K. Muzio, M.S. Nam, J. Nichol, R.J. Novikov, A. Nozdrina, A. Oberla, E. Pan, Y. Pfendner, C. Punsuebsay, N. Roth, J. Salcedo-Gomez, A. Seckel, D. Seikh, M.F.H. Shiao, Y.-S. Smith, D. Toscano, S. Torres, J. Touart, J. van Eijndhoven, N. Varner, G.S. Vieregg, A. Wang, M.-Z. Wang, S.-H. Wissel, S.A. Xie, C. Yoshida, S. Young, R. Université Libre de Bruxelles Science Faculty CP230 BrusselsB-1050 Belgium Department of Astronomy and Astrophysics Pennsylvania State University University ParkPA16802 United States Department of Physics Pennsylvania State University University ParkPA16802 United States Institute of Gravitation and the Cosmos Center for Multi-Messenger Astrophysics Pennsylvania State University University ParkPA16802 United States Dept. of Physics and Astronomy University of Kansas LawrenceKS66045 United States Dept. of Physics Center for Cosmology and AstroParticle Physics The Ohio State University ColumbusOH43210 United States Dept. of Physics Chiba University Chiba Japan Dept. of Physics University of Wisconsin-Madison MadisonWI53706 United States Dept. of Physics Grad. Inst. of Astrophys. Leung Center for Cosmology and Particle Astrophysics National Taiwan University Taipei Taiwan Dept. of Physics University of Maryland College ParkMD20742 United States Dept. of Physics Enrico Fermi Institue Kavli Institute for Cosmological Physics University of Chicago ChicagoIL60637 United States Dept. of Physics and Astronomy University College London London United Kingdom Center for Multi-Messenger Astrophysics Institute for Gravitation and the Cosmos Pennsylvania State University University ParkPA16802 United States Dept. of Physics Pennsylvania State University University ParkPA16802 United States Dept. of Astronomy and Astrophysics Pennsylvania State University University ParkPA16802 United States Vrije Universiteit Brussel Brussels Belgium Dept. of Physics and Astronomy University of Nebraska LincolnNE68588 United States Dept. Physics and Astronomy Whittier College WhittierCA90602 United States Dept. of Physics University of Delaware NewarkDE19716 United States Dept. of Energy Engineering National United University Miaoli Taiwan Dept. of Applied Physics National Pingtung University Pingtung County Pingtung City900393 Taiwan Dept. of Ph

The Askaryan Radio Array (ARA) is an in-ice ultrahigh energy (UHE, > 10 PeV) neutrino experiment at the South Pole that aims to detect radio emissions from neutrino-induced particle cascades. ARA has five independent stations which together have collected nearly 24 station-years of data. Each of these stations search for UHE neutrinos by burying in-ice clusters of antennas ∼200 m deep in a roughly cubical lattice with side length ∼15 m. Additionally, the fifth ARA station (A5) has a beamforming trigger, referred to as the Phased Array (PA), consisting of a trigger array of 7 tightly packed vertically-polarized antennas. In this proceeding, we will present a neutrino search with the data of this "hybrid" station, emphasizing its capabilities for improved analysis efficiencies, background rejection, and neutrino vertex reconstruction. This is enabled by combining the closely packed trigger antennas with the long-baselines of the outrigger antennas. We will also place the A5 analysis into the context of the broader five station analysis program, including efforts to characterize and calibrate the detector, model and constrain backgrounds, and reject noise across the entire array. We anticipate this full neutrino search to set world-leading limits above 100 PeV, and inform the next generation of neutrino detection experiments. © 2023, CC BY.

关键词： Neutrons

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Electromagnetic modeling and science reach of DMRadio-m3

arXiv

引用

arXiv 2023年

作者： AlShirawi, A. Bartram, C. Benabou, J.N. Brouwer, L. Chaudhuri, S. Cho, H.-M. Corbin, J. Craddock, W. Droster, A. Foster, J.W. Fry, J.T. Graham, P.W. Henning, R. Irwin, K.D. Kadribasic, F. Kahn, Y. Keller, A. Kolevatov, R. Kuenstner, S. Kurita, N. Leder, A.F. Li, D. Ouellet, J.L. Pappas, K.M.W. Phipps, A. Rapidis, N.M. Safdi, B.R. Salemi, C.P. Simanovskaia, M. Singh, J. van Assendelft, E.C. van Bibber, K. Wells, K. Winslow, L. Wisniewski, W.J. Young, B.A. Department of Physics Stanford University StanfordCA94305 United States SLAC National Accelerator Laboratory Menlo ParkCA94025 United States Kavli Institute for Particle Astrophysics and Cosmology Stanford University StanfordCA94305 United States Berkeley Center for Theoretical Physics University of California BerkeleyCA94720 United States Theoretical Physics Group Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Accelerator Techology and Applied Physics Division Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Department of Physics Princeton University PrincetonNJ08544 United States Department of Nuclear Engineering University of California Berkeley BerkeleyCA94720 United States Center for Theoretical Physics Massachusetts Institute of Technology CambridgeMA02139 United States Laboratory of Nuclear Science Massachusetts Institute of Technology CambridgeMA02139 United States Department of Physics and Astronomy University of North Carolina Chapel Hill Chapel HillNC27599 United States Triangle Universities Nuclear Laboratory DurhamNC27710 United States Department of Physics University of Illinois at Urbana-Champaign UrbanaIL61801 United States Physics Division Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Department of Physics California State University East Bay HaywardCA94542 United States Department of Physics Santa Clara University Santa ClaraCA95053 United States

DMRadio-m3 is an experiment that is designed to be sensitive to KSVZ and DFSZ QCD axion models in the 10–200 MHz (41 neV/c2 – 0.83 µeV/c2) range. The experiment uses a solenoidal dc magnetic field to convert an axion dark-matter signal to an ac electromagnetic response in a coaxial copper pickup. The current induced by this axion signal is measured by dc SQUIDs. In this work, we present the electromagnetic modeling of the response of the experiment to an axion signal over the full frequency range of DMRadio-m3, which extends from the low-frequency, lumped-element limit to a regime where the axion Compton wavelength is only a factor of two larger than the detector size. With these results, we determine the live time and sensitivity of the experiment. The primary science goal of sensitivity to DFSZ axions across 30–200 MHz can be achieved with a 3σ live scan time of 3.7 years. © 2023, CC BY.

关键词： Computational electromagnetics

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Chiral crossover transition from the Dyson-Schwinger equations in a sphere

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Physical Review D 2020年第11期102卷 114011-114011页

作者： Yin-Zhen Xu Chao Shi Xiao-Tao He Hong-Shi Zong Department of Physics Nanjing University Nanjing 210093 China Department of Nuclear Science and Technology Nanjing University of Aeronautics and Astronautics Nanjing 210016 China Department of Physics Anhui Normal University Wuhu 241000 China Nanjing Proton Source Research and Design Center Nanjing 210093 China Joint Center for Particle Nuclear Physics and Cosmology Nanjing 210093 China

Within the framework of Dyson-Schwinger equations of QCD, we study the effect of finite volume on the chiral phase transition in a sphere with the MIT boundary condition. We find that the chiral quark condensate ⟨ψ¯ψ⟩ and pseudotransition temperature Tpc of the crossover decreases as the volume decreases, until there is no chiral crossover transition at last. We find that the system for R=∞ fm is indistinguishable from R=10 fm and there is a significant decrease in Tpc with R as R<4 fm. When R<1.5 fm, there is no chiral transition in the system.

关键词： Nuclear matter QCD phase transitions

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The Minimum Variation Timescales of X-ray bursts from SGR J1935+2154

arXiv

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arXiv 2023年

作者： Xiao, Shuo Yang, Jiao-Jiao Luo, Xi-Hong Xiong, Shao-Lin Qu, Yuan-Hong Zhang, Shuang-Nan Xue, Wang-Chen Li, Xiao-Bo Tuo, You-Li Dong, Ai-Jun Zhao, Ru-Shuang Dang, Shi-Jun Shang, Lun-Hua Ma, Qing-Bo Cai, Ce Wang, Jin Wang, Ping Li, Cheng-Kui Yi, Shu-Xu Zhang, Zhen Ge, Ming-Yu Zheng, Shi-Jie Song, Li-Ming Peng, Wen-Xi Wen, Xiang-Yang Li, Xin-Qiao An, Zheng-Hua Xu, Xin Wang, Yue Zheng, Chao Zhang, Yan-Qiu Liu, Jia-Cong Zhang, Bin Xie, Wei Feng, Jian-Chao Wang, De-Hua Zhi, Qi-Jun Guizhou Provincial Key Laboratory of Radio Astronomy and Data Processing Guizhou Normal University Guiyang550001 China School of Physics and Electronic Science Guizhou Normal University Guiyang550001 China Key Laboratory of Particle Astrophysics Institute of High Energy Physics Chinese Academy of Sciences Beijing100049 China Nevada Center for Astrophysics University of Nevada Las VegasNV89154 United States Department of Physics and Astronomy University of Nevada Las Vegas Las VegasNV89154 United States University of Chinese Academy of Sciences Chinese Academy of Sciences Beijing100049 China Institut für Astronomie und Astrophysik University of Tübingen Sand 1 Tübingen72076 Germany College of Physics Hebei Normal University 20 South Erhuan Road Shijiazhuang050024 China

The minimum variation timescale (MVT) of soft gamma-ray repeaters can be an important probe to estimate the emission region in pulsar-like models, as well as the Lorentz factor and radius of the possible relativistic jet in gamma-ray burst (GRB)-like models, thus revealing their progenitors and physical mechanisms. In this work, we systematically study the MVTs of hundreds of X-ray bursts (XRBs) from SGR J1935+2154 observed by Insight-HXMT, GECAM and Fermi/GBM from July 2014 to Jan 2022 through the Bayesian Block algorithm. We find that the MVTs peak at ∼ 2 ms, corresponding to a light travel time size of about 600 km, which supports the magnetospheric origin in pulsar-like models. The shock radius and the Lorentz factor of the jet are also constrained in GRB-like models. Interestingly, the MVT of the XRB associated with FRB 200428 is ∼ 70 ms, which is longer than that of most bursts and implies its special radiation mechanism. Besides, the median of MVTs is 7 ms, shorter than the median MVTs of 40 ms and 480 ms for short GRBs or long GRBs, respectively. However, the MVT is independent of duration, similar to GRBs. Finally, we investigate the energy dependence of MVT and suggest that there is a marginal evidence for a power-law relationship like GRBs but the rate of variation is at least about an order of magnitude smaller. These features may provide an approach to identify bursts with a magnetar origin. © 2023, CC BY-SA.

关键词： Pulsars

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