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Álvarez-Domínguez Á, Garay LJ, Martín-Martínez E, Polo-Gómez J. No Black Holes from Light. PHYSICAL REVIEW LETTERS 2024; 133:041401. [PMID: 39121419 DOI: 10.1103/physrevlett.133.041401] [Citation(s) in RCA: 1] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/04/2024] [Accepted: 06/07/2024] [Indexed: 08/11/2024]
Abstract
We show that it is not possible to concentrate enough light to precipitate the formation of an event horizon. We argue that the dissipative quantum effects coming from the self-interaction of light (such as vacuum polarization) are enough to prevent any meaningful buildup of energy that could create a black hole in any realistic scenario.
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Affiliation(s)
| | | | - Eduardo Martín-Martínez
- Department of Applied Mathematics, University of Waterloo, Waterloo, Ontario N2L 3G1, Canada
- Institute for Quantum Computing, University of Waterloo, Waterloo, Ontario N2L 3G1, Canada
- Perimeter Institute for Theoretical Physics, Waterloo, Ontario N2L 2Y5, Canada
| | - José Polo-Gómez
- Department of Applied Mathematics, University of Waterloo, Waterloo, Ontario N2L 3G1, Canada
- Institute for Quantum Computing, University of Waterloo, Waterloo, Ontario N2L 3G1, Canada
- Perimeter Institute for Theoretical Physics, Waterloo, Ontario N2L 2Y5, Canada
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Arrowsmith CD, Simon P, Bilbao PJ, Bott AFA, Burger S, Chen H, Cruz FD, Davenne T, Efthymiopoulos I, Froula DH, Goillot A, Gudmundsson JT, Haberberger D, Halliday JWD, Hodge T, Huffman BT, Iaquinta S, Miniati F, Reville B, Sarkar S, Schekochihin AA, Silva LO, Simpson R, Stergiou V, Trines RMGM, Vieu T, Charitonidis N, Bingham R, Gregori G. Laboratory realization of relativistic pair-plasma beams. Nat Commun 2024; 15:5029. [PMID: 38866733 PMCID: PMC11169600 DOI: 10.1038/s41467-024-49346-2] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 12/27/2023] [Accepted: 05/31/2024] [Indexed: 06/14/2024] Open
Abstract
Relativistic electron-positron plasmas are ubiquitous in extreme astrophysical environments such as black-hole and neutron-star magnetospheres, where accretion-powered jets and pulsar winds are expected to be enriched with electron-positron pairs. Their role in the dynamics of such environments is in many cases believed to be fundamental, but their behavior differs significantly from typical electron-ion plasmas due to the matter-antimatter symmetry of the charged components. So far, our experimental inability to produce large yields of positrons in quasi-neutral beams has restricted the understanding of electron-positron pair plasmas to simple numerical and analytical studies, which are rather limited. We present the first experimental results confirming the generation of high-density, quasi-neutral, relativistic electron-positron pair beams using the 440 GeV/c beam at CERN's Super Proton Synchrotron (SPS) accelerator. Monte Carlo simulations agree well with the experimental data and show that the characteristic scales necessary for collective plasma behavior, such as the Debye length and the collisionless skin depth, are exceeded by the measured size of the produced pair beams. Our work opens up the possibility of directly probing the microphysics of pair plasmas beyond quasi-linear evolution into regimes that are challenging to simulate or measure via astronomical observations.
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Affiliation(s)
- C D Arrowsmith
- Department of Physics, University of Oxford, Parks Road, Oxford, OX1 3PU, UK.
| | - P Simon
- European Organization for Nuclear Research (CERN), CH-1211, Geneva 23, Switzerland
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Planckstraße 1, 64291, Darmstadt, Germany
| | - P J Bilbao
- GoLP/Instituto de Plasmas e Fusão Nuclear, Instituto Superior Técnico, Universidade de Lisboa, 1049-001, Lisboa, Portugal
| | - A F A Bott
- Department of Physics, University of Oxford, Parks Road, Oxford, OX1 3PU, UK
| | - S Burger
- European Organization for Nuclear Research (CERN), CH-1211, Geneva 23, Switzerland
| | - H Chen
- Lawrence Livermore National Laboratory, 7000 East Ave, Livermore, CA, 94550, USA
| | - F D Cruz
- GoLP/Instituto de Plasmas e Fusão Nuclear, Instituto Superior Técnico, Universidade de Lisboa, 1049-001, Lisboa, Portugal
| | - T Davenne
- STFC Rutherford Appleton Laboratory, Chilton, Didcot, OX11 0QX, UK
| | - I Efthymiopoulos
- European Organization for Nuclear Research (CERN), CH-1211, Geneva 23, Switzerland
| | - D H Froula
- University of Rochester Laboratory for Laser Energetics, Rochester, NY, 14623, USA
| | - A Goillot
- European Organization for Nuclear Research (CERN), CH-1211, Geneva 23, Switzerland
| | - J T Gudmundsson
- Science Institute, University of Iceland, Dunhaga 3, IS-107, Reykjavik, Iceland
- Division of Space and Plasma Physics, School of Electrical Engineering and Computer Science, KTH Royal Institute of Technology, SE-100 44, Stockholm, Sweden
| | - D Haberberger
- University of Rochester Laboratory for Laser Energetics, Rochester, NY, 14623, USA
| | - J W D Halliday
- Department of Physics, University of Oxford, Parks Road, Oxford, OX1 3PU, UK
| | - T Hodge
- Department of Physics, University of Oxford, Parks Road, Oxford, OX1 3PU, UK
- AWE, Aldermaston, Reading, Berkshire, RG7 4PR, UK
| | - B T Huffman
- Department of Physics, University of Oxford, Parks Road, Oxford, OX1 3PU, UK
| | - S Iaquinta
- Department of Physics, University of Oxford, Parks Road, Oxford, OX1 3PU, UK
| | - F Miniati
- Department of Physics, University of Oxford, Parks Road, Oxford, OX1 3PU, UK
| | - B Reville
- Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, D-69117, Heidelberg, Germany
| | - S Sarkar
- Department of Physics, University of Oxford, Parks Road, Oxford, OX1 3PU, UK
| | - A A Schekochihin
- Department of Physics, University of Oxford, Parks Road, Oxford, OX1 3PU, UK
| | - L O Silva
- GoLP/Instituto de Plasmas e Fusão Nuclear, Instituto Superior Técnico, Universidade de Lisboa, 1049-001, Lisboa, Portugal
| | - R Simpson
- Lawrence Livermore National Laboratory, 7000 East Ave, Livermore, CA, 94550, USA
| | - V Stergiou
- Department of Physics, University of Oxford, Parks Road, Oxford, OX1 3PU, UK
- European Organization for Nuclear Research (CERN), CH-1211, Geneva 23, Switzerland
- School of Applied Mathematics and Physical Sciences, National Technical University of Athens, Athens, 157 72, Greece
| | - R M G M Trines
- STFC Rutherford Appleton Laboratory, Chilton, Didcot, OX11 0QX, UK
| | - T Vieu
- Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, D-69117, Heidelberg, Germany
| | - N Charitonidis
- European Organization for Nuclear Research (CERN), CH-1211, Geneva 23, Switzerland
| | - R Bingham
- STFC Rutherford Appleton Laboratory, Chilton, Didcot, OX11 0QX, UK
- Department of Physics, University of Strathclyde, Glasgow, G4 0NG, UK
| | - G Gregori
- Department of Physics, University of Oxford, Parks Road, Oxford, OX1 3PU, UK
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New Developments in Relativistic Magnetohydrodynamics. Symmetry (Basel) 2022. [DOI: 10.3390/sym14091851] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/16/2022] Open
Abstract
Relativistic magnetohydrodynamics (RMHD) provides an extremely useful description of the low-energy long-wavelength phenomena in a variety of physical systems from quark–gluon plasma in heavy-ion collisions to matters in supernova, compact stars, and early universe. We review the recent theoretical progresses of RMHD, such as a formulation of RMHD from the perspective of magnetic flux conservation using the entropy–current analysis, the nonequilibrium statistical operator approach applied to quantum electrodynamics, and the relativistic kinetic theory. We discuss how the transport coefficients in RMHD are computed in kinetic theory and perturbative quantum field theories. We also explore the collective modes and instabilities in RMHD with a special emphasis on the role of chirality in a parity-odd plasma. We also give some future prospects of RMHD, including the interaction with spin hydrodynamics and the new kinetic framework with magnetic flux conservation.
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Magnetic Field Evolution in Neutron Star Crusts: Beyond the Hall Effect. Symmetry (Basel) 2022. [DOI: 10.3390/sym14010130] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 02/05/2023] Open
Abstract
Neutron stars host the strongest magnetic fields that we know of in the Universe. Their magnetic fields are the main means of generating their radiation, either magnetospheric or through the crust. Moreover, the evolution of the magnetic field has been intimately related to explosive events of magnetars, which host strong magnetic fields, and their persistent thermal emission. The evolution of the magnetic field in the crusts of neutron stars has been described within the framework of the Hall effect and Ohmic dissipation. Yet, this description is limited by the fact that the Maxwell stresses exerted on the crusts of strongly magnetised neutron stars may lead to failure and temperature variations. In the former case, a failed crust does not completely fulfil the necessary conditions for the Hall effect. In the latter, the variations of temperature are strongly related to the magnetic field evolution. Finally, sharp gradients of the star’s temperature may activate battery terms and alter the magnetic field structure, especially in weakly magnetised neutron stars. In this review, we discuss the recent progress made on these effects. We argue that these phenomena are likely to provide novel insight into our understanding of neutron stars and their observable properties.
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Abstract
Probing the existence of hypothetical particles beyond the Standard model often deals with extreme parameters: large energies, tiny cross-sections, large time scales, etc. Sometimes, laboratory experiments can test required regions of parameter space, but more often natural limitations lead to poorly restrictive upper limits. In such cases, astrophysical studies can help to expand the range of values significantly. Among astronomical sources, used in interests of fundamental physics, compact objects—neutron stars and white dwarfs—play a leading role. We review several aspects of astroparticle physics studies related to observations and properties of these celestial bodies. Dark matter particles can be collected inside compact objects resulting in additional heating or collapse. We summarize regimes and rates of particle capturing as well as possible astrophysical consequences. Then, we focus on a particular type of hypothetical particles—axions. Their existence can be uncovered due to observations of emission originated due to the Primakoff process in magnetospheres of neutron stars or white dwarfs. Alternatively, they can contribute to the cooling of these compact objects. We present results in these areas, including upper limits based on recent observations.
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Abstract
Neutron stars are natural physical laboratories allowing us to study a plethora of phenomena in extreme conditions. In particular, these compact objects can have very strong magnetic fields with non-trivial origin and evolution. In many respects, its magnetic field determines the appearance of a neutron star. Thus, understanding the field properties is important for the interpretation of observational data. Complementing this, observations of diverse kinds of neutron stars enable us to probe parameters of electro-dynamical processes at scales unavailable in terrestrial laboratories. In this review, we first briefly describe theoretical models of the formation and evolution of the magnetic field of neutron stars, paying special attention to field decay processes. Then, we present important observational results related to the field properties of different types of compact objects: magnetars, cooling neutron stars, radio pulsars, and sources in binary systems. After that, we discuss which observations can shed light on the obscure characteristics of neutron star magnetic fields and their behaviour. We end the review with a subjective list of open problems.
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Heinzl T, Ilderton A, King B. Classical Resummation and Breakdown of Strong-Field QED. PHYSICAL REVIEW LETTERS 2021; 127:061601. [PMID: 34420332 DOI: 10.1103/physrevlett.127.061601] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/05/2021] [Revised: 05/11/2021] [Accepted: 06/30/2021] [Indexed: 06/13/2023]
Abstract
QED perturbation theory has been conjectured to break down in sufficiently strong backgrounds, obstructing the analysis of strong-field physics. We show that the breakdown occurs even in classical electrodynamics, at lower field strengths than previously considered, and that it may be cured by resummation. As a consequence, an analogous resummation is required in QED. A detailed investigation shows, for a range of observables, that unitarity removes diagrams previously believed to be responsible for the breakdown of QED perturbation theory.
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Affiliation(s)
- T Heinzl
- Centre for Mathematical Sciences, University of Plymouth, Plymouth PL4 8AA, United Kingdom
| | - A Ilderton
- Centre for Mathematical Sciences, University of Plymouth, Plymouth PL4 8AA, United Kingdom
| | - B King
- Centre for Mathematical Sciences, University of Plymouth, Plymouth PL4 8AA, United Kingdom
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Murphy D, Mangan J, Ulyanov A, Walsh S, Dunwoody R, Hanlon L, Shortt B, McBreen S. Balloon flight test of a CeBr 3 detector with silicon photomultiplier readout. EXPERIMENTAL ASTRONOMY 2021; 52:1-34. [PMID: 34744307 PMCID: PMC8556215 DOI: 10.1007/s10686-021-09767-z] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 01/29/2021] [Accepted: 05/26/2021] [Indexed: 06/13/2023]
Abstract
Recent advances in silicon photomultiplier (SiPM) technology and new scintillator materials allow for the creation of compact high-performance gamma-ray detectors which can be deployed on small low-cost satellites. A small number of such satellites can provide full sky coverage and complement, or in some cases replace the existing gamma-ray missions in detection of transient gamma-ray events. The aim of this study is to test gamma-ray detection using a novel commercially available CeBr3 scintillator combined with SiPM readout in a near-space environment and inform further technology development for a future space mission. A prototype gamma-ray detector was built using a CeBr3 scintillator and an array of 16 J-Series SiPMs by ON Semiconductor. SiPM readout was performed using SIPHRA, a radiation-tolerant low-power integrated circuit developed by IDEAS. The detector was flown as a piggyback payload on the Advanced Scintillator Compton Telescope balloon flight from Columbia Scientific Balloon Facility. The payload included the detector, a Raspberry Pi on-board computer, a custom power supply board, temperature and pressure sensors, a Global Navigation Satellite System receiver and a satellite modem. The balloon delivered the detector to 37 km altitude where its detection capabilities and readout were tested in the radiation-intense near-space environment. The detector demonstrated continuous operation during the 8-hour flight and after the landing. It performed spectral measurements in an energy range of 100 keV to 8 MeV and observed the 511 keV gamma-ray line arising from positron annihilation in the atmosphere with full width half maximum of 6.8%. During ascent and descent, the detector count rate peaked at an altitude of 16 km corresponding to the point of maximum radiation intensity in the atmosphere. Despite several engineering issues discovered after the flight test, the results of this study confirm the feasibility of using CeBr3 scintillator, SiPMs, and SIPHRA in future space missions.
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Affiliation(s)
- David Murphy
- School of Physics and Centre for Space Research, University College Dublin, Dublin 4, Ireland
| | - Joseph Mangan
- School of Physics and Centre for Space Research, University College Dublin, Dublin 4, Ireland
| | - Alexei Ulyanov
- School of Physics and Centre for Space Research, University College Dublin, Dublin 4, Ireland
| | - Sarah Walsh
- School of Physics and Centre for Space Research, University College Dublin, Dublin 4, Ireland
| | - Rachel Dunwoody
- School of Physics and Centre for Space Research, University College Dublin, Dublin 4, Ireland
| | - Lorraine Hanlon
- School of Physics and Centre for Space Research, University College Dublin, Dublin 4, Ireland
| | - Brian Shortt
- European Space Agency, ESTEC, 2200 AG Noordwijk, The Netherlands
| | - Sheila McBreen
- School of Physics and Centre for Space Research, University College Dublin, Dublin 4, Ireland
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Enoto T, Kisaka S, Shibata S. Observational diversity of magnetized neutron stars. REPORTS ON PROGRESS IN PHYSICS. PHYSICAL SOCIETY (GREAT BRITAIN) 2019; 82:106901. [PMID: 31549688 DOI: 10.1088/1361-6633/ab3def] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/10/2023]
Abstract
Young and rotation-powered neutron stars (NSs) are commonly observed as rapidly-spinning pulsars. They dissipate their rotational energy by emitting pulsar wind with electromagnetic radiation and spin down at a steady rate, according to the simple steadily-rotating magnetic dipole model. In reality, however, multiwavelength observations of radiation from the NS surface and magnetosphere have revealed that the evolution and properties of NSs are highly diverse, often dubbed as 'NS zoo'. In particular, many of young and highly magnetized NSs show a high degree of activities, such as sporadic electromagnetic outbursts and irregular changes in pulse arrival times. Importantly, their magnetic field, which are the strongest in the universe, makes them ideal laboratories for fundamental physics. A class of highly-magnetized isolated NSs is empirically divided into several subclasses. In a broad classification, they are, in the order of the magnetic field strength (B) from the highest, 'magnetars' (historically recognized as soft gamma-ray repeaters and/or anomalous x-ray pulsars), 'high-B pulsars', and (nearby) x-ray isolated NSs. This article presents an introductory review for non-astrophysicists about the observational properties of highly-magnetized NSs, and their implications. The observed dynamic nature of NSs must be interpreted in conjunction with transient magnetic activities triggered during magnetic-energy dissipation process. In particular, we focus on how the five fundamental quantities of NSs, i.e. mass, radius, spin period, surface temperature, and magnetic fields, as observed with modern instruments, change with evolution of, and vary depending on the class of, the NSs. They are the foundation for a future unified theory of NSs.
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Affiliation(s)
- Teruaki Enoto
- Department of Astronomy and The Hakubi Center for Advanced Research, Kyoto University, Kyoto 606-8302, Japan
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Instrumentation and Future Missions in the Upcoming Era of X-ray Polarimetry. GALAXIES 2018. [DOI: 10.3390/galaxies6020054] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
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Gould O, Rajantie A. Magnetic Monopole Mass Bounds from Heavy-Ion Collisions and Neutron Stars. PHYSICAL REVIEW LETTERS 2017; 119:241601. [PMID: 29286728 DOI: 10.1103/physrevlett.119.241601] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/22/2017] [Indexed: 06/07/2023]
Abstract
Magnetic monopoles, if they exist, would be produced amply in strong magnetic fields and high temperatures via the thermal Schwinger process. Such circumstances arise in heavy-ion collisions and in neutron stars, both of which imply lower bounds on the mass of possible magnetic monopoles. In showing this, we construct the cross section for pair production of magnetic monopoles in heavy-ion collisions, which indicates that they are particularly promising for experimental searches such as MoEDAL.
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Affiliation(s)
- Oliver Gould
- Department of Physics, Imperial College London, London SW7 2AZ, United Kingdom
| | - Arttu Rajantie
- Department of Physics, Imperial College London, London SW7 2AZ, United Kingdom
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THE EINSTEIN@HOME GAMMA-RAY PULSAR SURVEY. I. SEARCH METHODS, SENSITIVITY, AND DISCOVERY OF NEW YOUNG GAMMA-RAY PULSARS. ACTA ACUST UNITED AC 2017. [DOI: 10.3847/1538-4357/834/2/106] [Citation(s) in RCA: 43] [Impact Index Per Article: 6.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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Belyaev V, Gvozdev A. Direct URCA-processes in neutron star quark core with strong magnetic field. EPJ WEB OF CONFERENCES 2017. [DOI: 10.1051/epjconf/201715805003] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
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EQUATION OF STATE FOR NUCLEONIC AND HYPERONIC NEUTRON STARS WITH MASS AND RADIUS CONSTRAINTS. ACTA ACUST UNITED AC 2016. [DOI: 10.3847/1538-4357/834/1/3] [Citation(s) in RCA: 65] [Impact Index Per Article: 8.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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Huang XG. Electromagnetic fields and anomalous transports in heavy-ion collisions-a pedagogical review. REPORTS ON PROGRESS IN PHYSICS. PHYSICAL SOCIETY (GREAT BRITAIN) 2016; 79:076302. [PMID: 27275776 DOI: 10.1088/0034-4885/79/7/076302] [Citation(s) in RCA: 15] [Impact Index Per Article: 1.9] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/06/2023]
Abstract
The hot and dense matter generated in heavy-ion collisions may contain domains which are not invariant under P and CP transformations. Moreover, heavy-ion collisions can generate extremely strong magnetic fields as well as electric fields. The interplay between the electromagnetic field and triangle anomaly leads to a number of macroscopic quantum phenomena in these P- and CP-odd domains known as anomalous transports. The purpose of this article is to give a pedagogical review of various properties of the electromagnetic fields, the anomalous transport phenomena, and their experimental signatures in heavy-ion collisions.
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Affiliation(s)
- Xu-Guang Huang
- Physics Department and Center for Particle Physics and Field Theory, Fudan University, Shanghai 200433, People's Republic of China
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Ma G, Yu W, Yu MY, Luan S, Wu D. Control of transmission of right circularly polarized laser light in overdense plasma by applied magnetic field pulses. Phys Rev E 2016; 93:053209. [PMID: 27300997 DOI: 10.1103/physreve.93.053209] [Citation(s) in RCA: 11] [Impact Index Per Article: 1.4] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/17/2016] [Indexed: 11/07/2022]
Abstract
The effect of a transient magnetic field on right-hand circularly polarized (RHCP) laser light propagation in overcritical-density plasma is investigated. When the electron gyrofrequency is larger than the wave frequency, RHCP light can propagate along the external magnetic field in an overcritical density plasma without resonance or cutoff. However, when the magnetic field falls to below the cyclotron resonance point, the propagating laser pulse will be truncated and the local plasma electrons resonantly heated. Particle-in-cell simulation shows that when applied to a thin slab, the process can produce intense two-cycle light pulses as well as long-lasting self-magnetic fields.
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Affiliation(s)
- Guangjin Ma
- State Key Laboratory of High Field Laser Physics, Shanghai Institute of Optics and Fine Mechanics, Chinese Academy of Sciences, Shanghai 201800, China
| | - Wei Yu
- State Key Laboratory of High Field Laser Physics, Shanghai Institute of Optics and Fine Mechanics, Chinese Academy of Sciences, Shanghai 201800, China
| | - M Y Yu
- Institute for Fusion Theory and Simulation and Department of Physics, Zhejiang University, Hangzhou 310027, China.,Institut für Theoretische Physik I, Ruhr-Universität Bochum, D-44780 Bochum, Germany
| | - Shixia Luan
- State Key Laboratory of High Field Laser Physics, Shanghai Institute of Optics and Fine Mechanics, Chinese Academy of Sciences, Shanghai 201800, China
| | - Dong Wu
- State Key Laboratory of High Field Laser Physics, Shanghai Institute of Optics and Fine Mechanics, Chinese Academy of Sciences, Shanghai 201800, China.,Helmholtz Institute Jena, D-07743 Jena, Germany
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Dvornikov M. Relaxation of the chiral imbalance in dense matter of a neutron star. EPJ WEB OF CONFERENCES 2016. [DOI: 10.1051/epjconf/201612503017] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
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Dvornikov M. Relaxation of the chiral imbalance in dense matter of a neutron star. EPJ WEB OF CONFERENCES 2016. [DOI: 10.1051/epjconf/201612505003] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
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