51
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Cheung C, Parra-Martinez J, Rothstein IZ, Shah N, Wilson-Gerow J. Effective Field Theory for Extreme Mass Ratio Binaries. PHYSICAL REVIEW LETTERS 2024; 132:091402. [PMID: 38489645 DOI: 10.1103/physrevlett.132.091402] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/27/2023] [Accepted: 01/23/2024] [Indexed: 03/17/2024]
Abstract
We derive an effective field theory describing a pair of gravitationally interacting point particles in an expansion in their mass ratio, also known as the self-force (SF) expansion. The 0SF dynamics are trivially obtained to all orders in Newton's constant by the geodesic motion of the light body in a Schwarzschild background encoding the gravitational field of the heavy body. The corrections at 1SF and higher are generated by perturbations about this configuration-that is, the geodesic deviation of the light body and the fluctuation graviton-but crucially supplemented by an operator describing the recoil of the heavy body as it interacts with the smaller companion. Using this formalism we compute new results at third post-Minkowskian order for the conservative dynamics of a system of gravitationally interacting massive particles coupled to a set of additional scalar and vector fields.
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Affiliation(s)
- Clifford Cheung
- Walter Burke Institute for Theoretical Physics, California Institute of Technology, Pasadena, California 91125, USA
| | - Julio Parra-Martinez
- Walter Burke Institute for Theoretical Physics, California Institute of Technology, Pasadena, California 91125, USA
- Department of Physics and Astronomy, University of British Columbia, Vancouver, V6T 1Z1, Canada
| | - Ira Z Rothstein
- Department of Physics, Carnegie Mellon University, Pittsburgh, Pennsylvania 15213, USA
| | - Nabha Shah
- Walter Burke Institute for Theoretical Physics, California Institute of Technology, Pasadena, California 91125, USA
| | - Jordan Wilson-Gerow
- Walter Burke Institute for Theoretical Physics, California Institute of Technology, Pasadena, California 91125, USA
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52
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Dawel F, Wilzewski A, Herbers S, Pelzer L, Kramer J, Hild MB, Dietze K, Krinner L, Spethmann NCH, Schmidt PO. Coherent photo-thermal noise cancellation in a dual-wavelength optical cavity for narrow-linewidth laser frequency stabilisation. OPTICS EXPRESS 2024; 32:7276-7288. [PMID: 38439412 DOI: 10.1364/oe.516433] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/21/2023] [Accepted: 02/01/2024] [Indexed: 03/06/2024]
Abstract
Optical resonators are used for the realisation of ultra-stable frequency lasers. The use of high reflectivity multi-band coatings allows the frequency locking of several lasers of different wavelengths to a single cavity. While the noise processes for single wavelength cavities are well known, the correlation caused by multi-stack coatings has as yet not been analysed experimentally. In our work, we stabilise the frequency of a 729 nm and a 1069 nm laser to one mirror pair and determine the residual-amplitude modulation (RAM) and photo-thermal noise (PTN). We find correlations in PTN between the two lasers and observe coherent cancellation of PTN for the 1069 nm coating. We show that the fractional frequency instability of the 729 nm laser is limited by RAM at 1 × 10-14. The instability of the 1069 nm laser is at 3 × 10-15 close to the thermal noise limit of 1.5 × 10-15.
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53
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Martins C, Cooke R, Liske J, Murphy M, Noterdaeme P, Schmidt T, Alcaniz JS, Alves CS, Balashev S, Cristiani S, Di Marcantonio P, Génova Santos R, Gonçalves RS, González Hernández JI, Maiolino R, Marconi A, Marques CMJ, Melo e Sousa MAF, Nunes NJ, Origlia L, Péroux C, Vinzl S, Zanutta A. Cosmology and fundamental physics with the ELT-ANDES spectrograph. EXPERIMENTAL ASTRONOMY 2024; 57:5. [PMID: 39308933 PMCID: PMC11413136 DOI: 10.1007/s10686-024-09928-w] [Citation(s) in RCA: 1] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 11/28/2023] [Accepted: 01/30/2024] [Indexed: 09/25/2024]
Abstract
State-of-the-art 19th century spectroscopy led to the discovery of quantum mechanics, and 20th century spectroscopy led to the confirmation of quantum electrodynamics. State-of-the-art 21st century astrophysical spectrographs, especially ANDES at ESO's ELT, have another opportunity to play a key role in the search for, and characterization of, the new physics which is known to be out there, waiting to be discovered. We rely on detailed simulations and forecast techniques to discuss four important examples of this point: big bang nucleosynthesis, the evolution of the cosmic microwave background temperature, tests of the universality of physical laws, and a real-time model-independent mapping of the expansion history of the universe (also known as the redshift drift). The last two are among the flagship science drivers for the ELT. We also highlight what is required for the ESO community to be able to play a meaningful role in 2030s fundamental cosmology and show that, even if ANDES only provides null results, such 'minimum guaranteed science' will be in the form of constraints on key cosmological paradigms: these are independent from, and can be competitive with, those obtained from traditional cosmological probes.
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Affiliation(s)
- C.J.A.P. Martins
- Centro de Astrofísica da Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal
- Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal
| | - R. Cooke
- Centre for Extragalactic Astronomy, Durham University, Science Site, South Road, DH1 3LE Durham, UK
| | - J. Liske
- Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany
| | - M.T. Murphy
- Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Victoria 3122 Australia
| | - P. Noterdaeme
- Institut d’Astrophysique de Paris, UMR 7095, CNRS-SU, 98bis bd Arago, 75014 Paris, France
- French-Chilean Laboratory for Astronomy, IRL 3386, CNRS and U. de Chile, Casilla 36-D, Santiago, Chile
| | - T.M. Schmidt
- Observatoire Astronomique de l’Université de Genève, Chemin Pegasi 51, Sauverny, CH-1290 Switzerland
| | - J. S. Alcaniz
- Observatório Nacional, 20921-400 Rio de Janeiro, RJ Brazil
| | - C. S. Alves
- Centro de Astrofísica da Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal
- Department of Physics and Astronomy, University College London, Gower Street, London, WC1E 6BT UK
| | - S. Balashev
- Ioffe Institute, Polyteknicheskaya 26, 194021 Saint-Petersburg, Russia
| | - S. Cristiani
- INAF–Osservatorio Astronomico di Trieste, Via G.B. Tiepolo, 11, I-34143 Trieste, Italy
- IFPU–Institute for Fundamental Physics of the Universe, via Beirut 2, I-34151 Trieste, Italy
- INFN-National Institute for Nuclear Physics, via Valerio 2, I-34127 Trieste, Italy
| | - P. Di Marcantonio
- INAF–Osservatorio Astronomico di Trieste, Via G.B. Tiepolo, 11, I-34143 Trieste, Italy
| | - R. Génova Santos
- Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife Spain
- Universidad de La Laguna, Department Astrofísica, E-38206 La Laguna, Tenerife Spain
| | - R. S. Gonçalves
- Observatório Nacional, 20921-400 Rio de Janeiro, RJ Brazil
- Departamento de Física, Universidade Federal Rural do Rio de Janeiro, 23897-000 Seropédica, RJ Brazil
| | - J. I. González Hernández
- Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife Spain
- Universidad de La Laguna, Department Astrofísica, E-38206 La Laguna, Tenerife Spain
| | - R. Maiolino
- Cavendish Laboratory, University of Cambridge, 19 J.J. Thomson Ave., Cambridge, CB3 0HE UK
| | - A. Marconi
- Dipartimento di Fisica e Astronomia, Universitaà degli Studi di Firenze, Via G. Sansone 1, Sesto Fiorentino, I-50019 Firenze, Italy
| | - C. M. J. Marques
- Centro de Astrofísica da Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal
- Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal
- Faculdade de Ciências, Universidade do Porto, Rua do Campo Alegre, 4150-007 Porto, Portugal
| | - M. A. F. Melo e Sousa
- Centro de Astrofísica da Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal
- Faculdade de Ciências, Universidade do Porto, Rua do Campo Alegre, 4150-007 Porto, Portugal
| | - N. J. Nunes
- Instituto de Astrofísica e Ciências do Espaço, Faculdade de Ciências da Universidade de Lisboa, Edifício C8, Campo Grande, 1749-016 Lisboa, Portugal
| | - L. Origlia
- INAF–Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, Via Gobetti 93/3, I-40129 Bologna, Italy
| | - C. Péroux
- European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching-bei-München, Germany
- Aix Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, 13388 Marseille, France
| | - S. Vinzl
- Université de Toulouse UPS, Toulouse, France
| | - A. Zanutta
- INAF–Osservatorio Astronomico di Brera, via E. Bianchi 46, 23807 Merate, Italy
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54
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Kartik YR, Kumar RR, Sarkar S. Critical scaling of a two-orbital topological model with extended neighboring couplings. Sci Rep 2024; 14:4504. [PMID: 38402262 PMCID: PMC10894280 DOI: 10.1038/s41598-024-54946-5] [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: 09/28/2023] [Accepted: 02/19/2024] [Indexed: 02/26/2024] Open
Abstract
Extended-range models are the interesting systems, which has been widely used to understand the non-local properties of the fermions at quantum scale. We aim to study the interplay between criticality and extended range couplings under various symmetry constraints. Here, we consider a two orbital Bernevig-Hughes-Zhang model in one dimension with longer (finite neighbor) and long-range (infinite neighbor) couplings. We study the behavior of model using scaling laws and universality class for models with Hermitian, parity-time ([Formula: see text]) symmetric and broken time-reversal symmetries. We observe the interesting results on multi-criticalities, where the universality class of critical exponent is different than the normal criticalities. Also, the results can be generalized by considering the interplay between criticalities and different symmetry classes of Hamiltonian. Also, with the introduction of extended-range of coupling, there occurs different criticalities, and we provide the analogy to characterize their universality classes. We also show the violation of Lorentz invariance at multi-criticalities and evaluation of short-range limit in long-range models as the highlights of this work.
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Affiliation(s)
- Y R Kartik
- Theoretical Sciences Division, Poornaprajna Institute of Scientific Research, Bidalur, Bengaluru, 562164, India
- Graduate Studies, Manipal Academy of Higher Education, Madhava Nagar, Manipal, 576104, India
| | - Ranjith R Kumar
- Theoretical Sciences Division, Poornaprajna Institute of Scientific Research, Bidalur, Bengaluru, 562164, India
- Graduate Studies, Manipal Academy of Higher Education, Madhava Nagar, Manipal, 576104, India
| | - Sujit Sarkar
- Theoretical Sciences Division, Poornaprajna Institute of Scientific Research, Bidalur, Bengaluru, 562164, India.
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55
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Franciolini G, Racco D, Rompineve F. Footprints of the QCD Crossover on Cosmological Gravitational Waves at Pulsar Timing Arrays. PHYSICAL REVIEW LETTERS 2024; 132:081001. [PMID: 38457711 DOI: 10.1103/physrevlett.132.081001] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/19/2023] [Revised: 12/01/2023] [Accepted: 01/24/2024] [Indexed: 03/10/2024]
Abstract
Pulsar timing arrays (PTAs) have reported evidence for a stochastic gravitational wave (GW) background at nanohertz frequencies, possibly originating in the early Universe. We show that the spectral shape of the low-frequency (causality) tail of GW signals sourced at temperatures around T≳1 GeV is distinctively affected by confinement of strong interactions (QCD), due to the corresponding sharp decrease in the number of relativistic species, and significantly deviates from ∼f^{3} commonly adopted in the literature. Bayesian analyses in the NANOGrav 15 years and the previous international PTA datasets reveal a significant improvement in the fit with respect to cubic power-law spectra, previously employed for the causality tail. While no conclusion on the nature of the signal can be drawn at the moment, our results show that the inclusion of standard model effects on cosmological GWs can have a decisive impact on model selection.
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Affiliation(s)
- Gabriele Franciolini
- Dipartimento di Fisica, Sapienza Università di Roma and INFN, Sezione di Roma, Piazzale Aldo Moro 5, 00185, Rome, Italy
| | - Davide Racco
- Stanford Institute for Theoretical Physics, Stanford University, 382 Via Pueblo Mall, Stanford, California 94305, USA
| | - Fabrizio Rompineve
- CERN, Theoretical Physics Department, Esplanade des Particules 1, Geneva 1211, Switzerland
- Departament de Física, Universitat Autònoma de Barcelona, 08193 Bellaterra, Barcelona, Spain
- Institut de Física d'Altes Energies (IFAE) and The Barcelona Institute of Science and Technology (BIST), Campus UAB, 08193 Bellaterra (Barcelona), Spain
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56
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Wang B, Abdalla E, Atrio-Barandela F, Pavón D. Further understanding the interaction between dark energy and dark matter: current status and future directions. REPORTS ON PROGRESS IN PHYSICS. PHYSICAL SOCIETY (GREAT BRITAIN) 2024; 87:036901. [PMID: 38306662 DOI: 10.1088/1361-6633/ad2527] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/06/2023] [Accepted: 02/02/2024] [Indexed: 02/04/2024]
Abstract
The interaction between dark matter and dark energy (DE) can be incorporated into field theory models of DE that have proved successful in alleviating the coincidence problem. We review recent advances in this field, including new models and constraints from different astronomical data sets. We show that interactions are allowed by observations and can reduce the current tensions among different measurements of cosmological parameters. We extend our discussion to include constraints from non-linear effects and results from cosmological simulations. Finally, we discuss forthcoming multi-messenger data from current and future observational facilities that will help to improve our understanding of the interactions within the dark sector.
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Affiliation(s)
- B Wang
- School of Aeronautics and Astronautics, Shanghai Jiao Tong University, Shanghai 200240, People's Republic of China
| | - E Abdalla
- Instituto de Fisica, Universidade de Sâo Paulo, Sâo Paulo, SP, Brazil
| | - F Atrio-Barandela
- Física Teórica, Universidad de Salamanca, Plaza de la Merced, Salamanca, Spain
| | - D Pavón
- Departamento de Física, Universidad Autónoma de Barcelona, Bellaterra, Barcelona, Spain
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57
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Charisi M, Taylor SR, Witt CA, Runnoe J. Efficient Large-Scale, Targeted Gravitational-Wave Probes of Supermassive Black-Hole Binaries. PHYSICAL REVIEW LETTERS 2024; 132:061401. [PMID: 38394573 DOI: 10.1103/physrevlett.132.061401] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/05/2023] [Revised: 10/27/2023] [Accepted: 11/21/2023] [Indexed: 02/25/2024]
Abstract
Binary systems of supermassive black holes are promising sources of low-frequency gravitational waves (GWs) and bright electromagnetic emission. Pulsar timing array GW searches for individual binaries have been limited to only a few candidate systems due to computational demands, which get worse as more pulsars are added. By modeling the GW signal using only components from when the GW passes Earth (rather than also each pulsar), we find constraints on the binary's total mass and GW frequency that are similar to a full signal analysis, yet ∼70 times more efficient.
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Affiliation(s)
- Maria Charisi
- Department of Physics and Astronomy, Vanderbilt University, 2301 Vanderbilt Place, Nashville, Tennessee 37235, USA
| | - Stephen R Taylor
- Department of Physics and Astronomy, Vanderbilt University, 2301 Vanderbilt Place, Nashville, Tennessee 37235, USA
| | - Caitlin A Witt
- Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA), Northwestern University, Evanston, Illinois 60208, USA
- Adler Planetarium, 1300 S. DuSable Lake Shore Drive, Chicago, Illinois 60605, USA
| | - Jessie Runnoe
- Department of Physics and Astronomy, Vanderbilt University, 2301 Vanderbilt Place, Nashville, Tennessee 37235, USA
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58
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De Falco V, Battista E, Usseglio D, Capozziello S. Radiative losses and radiation-reaction effects at the first post-Newtonian order in Einstein-Cartan theory. THE EUROPEAN PHYSICAL JOURNAL. C, PARTICLES AND FIELDS 2024; 84:137. [PMID: 39050376 PMCID: PMC11266255 DOI: 10.1140/epjc/s10052-024-12476-4] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 12/15/2023] [Accepted: 01/24/2024] [Indexed: 07/27/2024]
Abstract
Gravitational radiation-reaction phenomena occurring in the dynamics of inspiralling compact binary systems are investigated at the first post-Newtonian order beyond the quadrupole approximation in the context of Einstein-Cartan theory, where quantum spin effects are modeled via the Weyssenhoff fluid. We exploit balance equations for the energy and angular momentum to determine the binary orbital decay until the two bodies collide. Our framework deals with both quasi-elliptic and quasi-circular trajectories, which are then smoothly connected. Key observables like the laws of variation of the orbital phase and frequency characterizing the quasi-circular motion are derived analytically. We conclude our analysis with an estimation of the spin contributions at the merger, which are examined both in the time domain and the Fourier frequency space through the stationary wave approximation.
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Affiliation(s)
- Vittorio De Falco
- Scuola Superiore Meridionale, Largo San Marcellino 10, 80138 Naples, Italy
- Istituto Nazionale di Fisica Nucleare, Sezione di Napoli, Complesso Universitario di Monte S. Angelo, Via Cintia Edificio 6, 80126 Naples, Italy
| | - Emmanuele Battista
- Department of Physics, University of Vienna, Boltzmanngasse 5, 1090 Vienna, Austria
| | - Davide Usseglio
- Scuola Superiore Meridionale, Largo San Marcellino 10, 80138 Naples, Italy
- Istituto Nazionale di Fisica Nucleare, Sezione di Napoli, Complesso Universitario di Monte S. Angelo, Via Cintia Edificio 6, 80126 Naples, Italy
| | - Salvatore Capozziello
- Scuola Superiore Meridionale, Largo San Marcellino 10, 80138 Naples, Italy
- Istituto Nazionale di Fisica Nucleare, Sezione di Napoli, Complesso Universitario di Monte S. Angelo, Via Cintia Edificio 6, 80126 Naples, Italy
- Dipartimento di Fisica “E. Pancini”, Universitá di Napoli “Federico II”, Complesso Universitario di Monte S. Angelo, Via Cintia Edificio 6, 80126 Naples, Italy
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59
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Heisenberg L. Balance laws as test of gravitational waveforms. PHILOSOPHICAL TRANSACTIONS. SERIES A, MATHEMATICAL, PHYSICAL, AND ENGINEERING SCIENCES 2024; 382:20230086. [PMID: 38104623 DOI: 10.1098/rsta.2023.0086] [Citation(s) in RCA: 1] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/06/2023] [Accepted: 10/07/2023] [Indexed: 12/19/2023]
Abstract
Gravitational waveforms play a crucial role in comparing observed signals with theoretical predictions. However, obtaining accurate analytical waveforms directly from general relativity (GR) remains challenging. Existing methods involve a complex blend of post-Newtonian theory, effective-one-body formalism, numerical relativity and interpolation, introducing systematic errors. As gravitational wave astronomy advances with new detectors, these errors gain significance, particularly when testing GR in the nonlinear regime. A recent development proposes a novel approach to address this issue. By deriving precise constraints-or balance laws-directly from full nonlinear GR, this method offers a means to evaluate waveform quality, detect template weaknesses and ensure internal consistency. Before delving into the intricacies of balance laws in full nonlinear GR, we illustrate the concept using a detailed mechanical analogy. We will examine a dissipative mechanical system as an example, demonstrating how mechanical balance laws can gauge the accuracy of approximate solutions in capturing the complete physical scenario. While mechanical balance laws are straightforward, deriving balance laws in electromagnetism and GR demands a rigorous foundation rooted in mathematically precise concepts of radiation. Following the analogy with electromagnetism, we derive balance laws in GR. As a proof of concept, we employ an analytical approximate waveform model, showcasing how these balance laws serve as a litmus test for the model's validity. This article is part of the theme issue 'The particle-gravity frontier'.
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Affiliation(s)
- Lavinia Heisenberg
- Institute for Theoretical Physics, Philosophenweg 16, 69120 Heidelberg, Germany
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60
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Cannizzaro E, Sberna L, Green SR, Hollands S. Relativistic Perturbation Theory for Black-Hole Boson Clouds. PHYSICAL REVIEW LETTERS 2024; 132:051401. [PMID: 38364157 DOI: 10.1103/physrevlett.132.051401] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/02/2023] [Accepted: 12/15/2023] [Indexed: 02/18/2024]
Abstract
We develop a relativistic perturbation theory for scalar clouds around rotating black holes. We first introduce a relativistic product and corresponding orthogonality relation between modes, extending a recent result for gravitational perturbations. We then derive the analog of time-dependent perturbation theory in quantum mechanics, and apply it to calculate self-gravitational frequency shifts. This approach supersedes the nonrelativistic "gravitational atom" approximation, brings close agreement with numerical relativity, and has practical applications for gravitational-wave astronomy.
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Affiliation(s)
- Enrico Cannizzaro
- Dipartimento di Fisica, "Sapienza" Università di Roma & Sezione INFN Roma1, Piazzale Aldo Moro 5, 00185, Roma, Italy
| | - Laura Sberna
- Max Planck Institute for Gravitational Physics (Albert Einstein Institute) Am Muühlenberg 1, 14476 Potsdam, Germany
| | - Stephen R Green
- School of Mathematical Sciences, University of Nottingham, University Park, Nottingham NG7 2RD, United Kingdom
| | - Stefan Hollands
- Institut für Theoretische Physik, Universität Leipzig, Brüderstrasse 16, D-04103 Leipzig, Germany
- Max Planck Institute for Mathematics in the Sciences, Inselstrasse 16, D-04109 Leipzig, Germany
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61
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Burgess C, Patrick S, Torres T, Gregory R, König F. Quasinormal Modes of Optical Solitons. PHYSICAL REVIEW LETTERS 2024; 132:053802. [PMID: 38364120 DOI: 10.1103/physrevlett.132.053802] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/22/2023] [Accepted: 01/02/2024] [Indexed: 02/18/2024]
Abstract
Quasinormal modes (QNMs) are essential for understanding the stability and resonances of open systems, with increasing prominence in black hole physics. We present here the first study of QNMs of optical potentials. We show that solitons can support QNMs, deriving a soliton perturbation equation and giving exact analytical expressions for the QNMs of fiber solitons. We discuss the boundary conditions in this intrinsically dispersive system and identify novel signatures of dispersion. From here, we discover a new analogy with black holes and describe a regime in which the soliton is a robust black hole simulator for light-ring phenomena. Our results invite a range of applications, from the description of optical pulse propagation with QNMs to the use of state-of-the-art technology from fiber optics to address questions in black hole physics, such as QNM spectral instabilities and the role of nonlinearities in ringdown.
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Affiliation(s)
- Christopher Burgess
- School of Physics and Astronomy, SUPA, University of St. Andrews, North Haugh, St. Andrews, KY16 9SS, United Kingdom
| | - Sam Patrick
- Department of Physics, King's College London, The Strand, London, WC2R 2LS, United Kingdom
| | - Theo Torres
- Department of Physics, King's College London, The Strand, London, WC2R 2LS, United Kingdom
| | - Ruth Gregory
- Department of Physics, King's College London, The Strand, London, WC2R 2LS, United Kingdom
- Perimeter Institute, 31 Caroline Street North, Waterloo, Ontario N2L 2Y5, Canada
| | - Friedrich König
- School of Physics and Astronomy, SUPA, University of St. Andrews, North Haugh, St. Andrews, KY16 9SS, United Kingdom
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62
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Penin AA, Su A. Effective Theory of Classical and Quantum Particle Dynamics in Rapidly Oscillating Fields. PHYSICAL REVIEW LETTERS 2024; 132:051601. [PMID: 38364132 DOI: 10.1103/physrevlett.132.051601] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/05/2023] [Revised: 12/21/2023] [Accepted: 01/09/2024] [Indexed: 02/18/2024]
Abstract
We study the large-scale dynamics of charged particles in a rapidly oscillating field and formulate its classical and quantum effective theory description. The high-order perturbative results for the effective action are presented. Remarkably, the action models the effects of post-Newtonian general relativity on the motion of nonrelativistic particles, with the values of the emergent curvature and speed of light determined by the field spatial distribution and frequency. Our results can be applied to a wide range of physical problems including the high-precision analysis and design of the charged particle traps and Floquet quantum materials.
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Affiliation(s)
- Alexander A Penin
- Department of Physics, University of Alberta, Edmonton, Alberta T6G 2J1, Canada
| | - Aneca Su
- Department of Physics, University of Alberta, Edmonton, Alberta T6G 2J1, Canada
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63
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Levan AJ, Gompertz BP, Salafia OS, Bulla M, Burns E, Hotokezaka K, Izzo L, Lamb GP, Malesani DB, Oates SR, Ravasio ME, Rouco Escorial A, Schneider B, Sarin N, Schulze S, Tanvir NR, Ackley K, Anderson G, Brammer GB, Christensen L, Dhillon VS, Evans PA, Fausnaugh M, Fong WF, Fruchter AS, Fryer C, Fynbo JPU, Gaspari N, Heintz KE, Hjorth J, Kennea JA, Kennedy MR, Laskar T, Leloudas G, Mandel I, Martin-Carrillo A, Metzger BD, Nicholl M, Nugent A, Palmerio JT, Pugliese G, Rastinejad J, Rhodes L, Rossi A, Saccardi A, Smartt SJ, Stevance HF, Tohuvavohu A, van der Horst A, Vergani SD, Watson D, Barclay T, Bhirombhakdi K, Breedt E, Breeveld AA, Brown AJ, Campana S, Chrimes AA, D'Avanzo P, D'Elia V, De Pasquale M, Dyer MJ, Galloway DK, Garbutt JA, Green MJ, Hartmann DH, Jakobsson P, Kerry P, Kouveliotou C, Langeroodi D, Le Floc'h E, Leung JK, Littlefair SP, Munday J, O'Brien P, Parsons SG, Pelisoli I, Sahman DI, Salvaterra R, Sbarufatti B, Steeghs D, Tagliaferri G, Thöne CC, de Ugarte Postigo A, Kann DA. Heavy-element production in a compact object merger observed by JWST. Nature 2024; 626:737-741. [PMID: 37879361 PMCID: PMC10881391 DOI: 10.1038/s41586-023-06759-1] [Citation(s) in RCA: 3] [Impact Index Per Article: 3.0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/03/2023] [Accepted: 10/17/2023] [Indexed: 10/27/2023]
Abstract
The mergers of binary compact objects such as neutron stars and black holes are of central interest to several areas of astrophysics, including as the progenitors of gamma-ray bursts (GRBs)1, sources of high-frequency gravitational waves (GWs)2 and likely production sites for heavy-element nucleosynthesis by means of rapid neutron capture (the r-process)3. Here we present observations of the exceptionally bright GRB 230307A. We show that GRB 230307A belongs to the class of long-duration GRBs associated with compact object mergers4-6 and contains a kilonova similar to AT2017gfo, associated with the GW merger GW170817 (refs. 7-12). We obtained James Webb Space Telescope (JWST) mid-infrared imaging and spectroscopy 29 and 61 days after the burst. The spectroscopy shows an emission line at 2.15 microns, which we interpret as tellurium (atomic mass A = 130) and a very red source, emitting most of its light in the mid-infrared owing to the production of lanthanides. These observations demonstrate that nucleosynthesis in GRBs can create r-process elements across a broad atomic mass range and play a central role in heavy-element nucleosynthesis across the Universe.
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Affiliation(s)
- Andrew J Levan
- Department of Astrophysics, Institute for Mathematics, Astrophysics and Particle Physics (IMAPP), Radboud University, Nijmegen, The Netherlands.
- Department of Physics, University of Warwick, Coventry, UK.
| | - Benjamin P Gompertz
- Institute for Gravitational Wave Astronomy, University of Birmingham, Birmingham, UK
- School of Physics and Astronomy, University of Birmingham, Birmingham, UK
| | - Om Sharan Salafia
- INAF - Osservatorio Astronomico di Brera, Merate, Italy
- INFN - Sezione di Milano Bicocca, Milano, Italy
| | - Mattia Bulla
- Department of Physics and Earth Science, University of Ferrara, Ferrara, Italy
- INFN - Sezione di Ferrara, Ferrara, Italy
- INAF - Osservatorio Astronomico d'Abruzzo, Teramo, Italy
| | - Eric Burns
- Department of Physics & Astronomy, Louisiana State University, Baton Rouge, LA, USA
| | - Kenta Hotokezaka
- Research Center for the Early Universe, Graduate School of Science, The University of Tokyo, Bunkyo, Japan
- Kavli IPMU (WPI), UTIAS, The University of Tokyo, Kashiwa, Chiba, Japan
| | - Luca Izzo
- DARK, Niels Bohr Institute, University of Copenhagen, Copenhagen N, Denmark
- INAF - Osservatorio Astronomico di Capodimonte, Naples, Italy
| | - Gavin P Lamb
- Astrophysics Research Institute, Liverpool John Moores University, Liverpool, UK
- School of Physics and Astronomy, University of Leicester, Leicester, UK
| | - Daniele B Malesani
- Department of Astrophysics, Institute for Mathematics, Astrophysics and Particle Physics (IMAPP), Radboud University, Nijmegen, The Netherlands
- Cosmic Dawn Center (DAWN), Copenhagen, Denmark
- Niels Bohr Institute, University of Copenhagen, Copenhagen N, Denmark
| | - Samantha R Oates
- Institute for Gravitational Wave Astronomy, University of Birmingham, Birmingham, UK
- School of Physics and Astronomy, University of Birmingham, Birmingham, UK
| | - Maria Edvige Ravasio
- Department of Astrophysics, Institute for Mathematics, Astrophysics and Particle Physics (IMAPP), Radboud University, Nijmegen, The Netherlands
- INAF - Osservatorio Astronomico di Brera, Merate, Italy
| | | | - Benjamin Schneider
- Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA, USA
| | - Nikhil Sarin
- Nordita, Stockholm University and KTH Royal Institute of Technology, Stockholm, Sweden
- The Oskar Klein Centre, Department of Physics, Stockholm University, AlbaNova University Center, Stockholm, Sweden
| | - Steve Schulze
- The Oskar Klein Centre, Department of Physics, Stockholm University, AlbaNova University Center, Stockholm, Sweden
| | - Nial R Tanvir
- School of Physics and Astronomy, University of Leicester, Leicester, UK
| | - Kendall Ackley
- Department of Physics, University of Warwick, Coventry, UK
| | - Gemma Anderson
- International Centre for Radio Astronomy Research, Curtin University, Perth, Western Australia, Australia
| | - Gabriel B Brammer
- Cosmic Dawn Center (DAWN), Copenhagen, Denmark
- Niels Bohr Institute, University of Copenhagen, Copenhagen N, Denmark
| | - Lise Christensen
- Cosmic Dawn Center (DAWN), Copenhagen, Denmark
- Niels Bohr Institute, University of Copenhagen, Copenhagen N, Denmark
| | - Vikram S Dhillon
- Department of Physics and Astronomy, University of Sheffield, Sheffield, UK
- Instituto de Astrofísica de Canarias, La Laguna, Tenerife, Spain
| | - Phil A Evans
- School of Physics and Astronomy, University of Leicester, Leicester, UK
| | - Michael Fausnaugh
- Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA, USA
- Department of Physics & Astronomy, Texas Tech University, Lubbock, TX, USA
| | - Wen-Fai Fong
- Center for Interdisciplinary Exploration and Research in Astrophysics, Northwestern University, Evanston, IL, USA
- Department of Physics and Astronomy, Northwestern University, Evanston, IL, USA
| | | | - Chris Fryer
- Center for Theoretical Astrophysics, Los Alamos National Laboratory, Los Alamos, NM, USA
- Department of Astronomy, The University of Arizona, Tucson, AZ, USA
- Department of Physics and Astronomy, The University of New Mexico, Albuquerque, NM, USA
- Department of Physics, The George Washington University, Washington, DC, USA
| | - Johan P U Fynbo
- Cosmic Dawn Center (DAWN), Copenhagen, Denmark
- Niels Bohr Institute, University of Copenhagen, Copenhagen N, Denmark
| | - Nicola Gaspari
- Department of Astrophysics, Institute for Mathematics, Astrophysics and Particle Physics (IMAPP), Radboud University, Nijmegen, The Netherlands
| | - Kasper E Heintz
- Cosmic Dawn Center (DAWN), Copenhagen, Denmark
- Niels Bohr Institute, University of Copenhagen, Copenhagen N, Denmark
| | - Jens Hjorth
- DARK, Niels Bohr Institute, University of Copenhagen, Copenhagen N, Denmark
| | - Jamie A Kennea
- Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA, USA
| | - Mark R Kennedy
- School of Physics, University College Cork, Cork, Ireland
- Jodrell Bank Centre for Astrophysics, Department of Physics and Astronomy, The University of Manchester, Manchester, UK
| | - Tanmoy Laskar
- Department of Astrophysics, Institute for Mathematics, Astrophysics and Particle Physics (IMAPP), Radboud University, Nijmegen, The Netherlands
- Department of Physics & Astronomy, University of Utah, Salt Lake City, UT, USA
| | - Giorgos Leloudas
- DTU Space, National Space Institute, Technical University of Denmark, Lyngby, Denmark
| | - Ilya Mandel
- School of Physics and Astronomy, Monash University, Clayton, Victoria, Australia
- ARC Centre of Excellence for Gravitational Wave Discovery (OzGrav), Monash University, Clayton, Victoria, Australia
| | | | - Brian D Metzger
- Columbia Astrophysics Laboratory, Department of Physics, Columbia University, New York, NY, USA
- Center for Computational Astrophysics, Flatiron Institute, New York, NY, USA
| | - Matt Nicholl
- Astrophysics Research Centre, School of Mathematics and Physics, Queen's University Belfast, Belfast, UK
| | - Anya Nugent
- Center for Interdisciplinary Exploration and Research in Astrophysics, Northwestern University, Evanston, IL, USA
- Department of Physics and Astronomy, Northwestern University, Evanston, IL, USA
| | - Jesse T Palmerio
- GEPI, Observatoire de Paris, Université PSL, CNRS, Meudon, France
| | - Giovanna Pugliese
- Anton Pannekoek Institute for Astronomy, University of Amsterdam, Amsterdam, The Netherlands
| | - Jillian Rastinejad
- Center for Interdisciplinary Exploration and Research in Astrophysics, Northwestern University, Evanston, IL, USA
- Department of Physics and Astronomy, Northwestern University, Evanston, IL, USA
| | - Lauren Rhodes
- Department of Physics, University of Oxford, Oxford, UK
| | - Andrea Rossi
- INAF - Osservatorio di Astrofisica e Scienza dello Spazio, Bologna, Italy
| | - Andrea Saccardi
- GEPI, Observatoire de Paris, Université PSL, CNRS, Meudon, France
| | - Stephen J Smartt
- Astrophysics Research Centre, School of Mathematics and Physics, Queen's University Belfast, Belfast, UK
- Department of Physics, University of Oxford, Oxford, UK
| | - Heloise F Stevance
- Department of Physics, University of Oxford, Oxford, UK
- Department of Physics, The University of Auckland, Auckland, New Zealand
| | - Aaron Tohuvavohu
- Department of Astronomy & Astrophysics, University of Toronto, Toronto, Ontario, Canada
| | | | | | - Darach Watson
- Cosmic Dawn Center (DAWN), Copenhagen, Denmark
- Niels Bohr Institute, University of Copenhagen, Copenhagen N, Denmark
| | | | | | - Elmé Breedt
- Institute of Astronomy, University of Cambridge, Cambridge, UK
| | - Alice A Breeveld
- Mullard Space Science Laboratory, University College London, Holmbury St. Mary, UK
| | - Alexander J Brown
- Department of Physics and Astronomy, University of Sheffield, Sheffield, UK
| | | | - Ashley A Chrimes
- Department of Astrophysics, Institute for Mathematics, Astrophysics and Particle Physics (IMAPP), Radboud University, Nijmegen, The Netherlands
| | | | - Valerio D'Elia
- Agenzia Spaziale Italiana (ASI) Space Science Data Center (SSDC), Rome, Italy
- INAF - Osservatorio Astronomico di Roma, Rome, Italy
| | - Massimiliano De Pasquale
- Department of Mathematics, Physics, Informatics and Earth Sciences, University of Messina, Polo Papardo, Messina, Italy
| | - Martin J Dyer
- Department of Physics and Astronomy, University of Sheffield, Sheffield, UK
| | - Duncan K Galloway
- School of Physics and Astronomy, Monash University, Clayton, Victoria, Australia
- ARC Centre of Excellence for Gravitational Wave Discovery (OzGrav), Monash University, Clayton, Victoria, Australia
| | - James A Garbutt
- Department of Physics and Astronomy, University of Sheffield, Sheffield, UK
| | - Matthew J Green
- School of Physics and Astronomy, Tel Aviv University, Tel Aviv, Israel
| | - Dieter H Hartmann
- Department of Physics and Astronomy, Clemson University, Clemson, SC, USA
| | - Páll Jakobsson
- Centre for Astrophysics and Cosmology, Science Institute, University of Iceland, Reykjavik, Iceland
| | - Paul Kerry
- Department of Physics and Astronomy, University of Sheffield, Sheffield, UK
| | - Chryssa Kouveliotou
- Department of Physics, The George Washington University, Washington, DC, USA
| | - Danial Langeroodi
- DARK, Niels Bohr Institute, University of Copenhagen, Copenhagen N, Denmark
| | - Emeric Le Floc'h
- CEA, IRFU, DAp, AIM, Université Paris-Saclay, Université Paris Cité, Sorbonne Paris Cité, CNRS, Gif-sur-Yvette, France
| | - James K Leung
- ARC Centre of Excellence for Gravitational Wave Discovery (OzGrav), Monash University, Clayton, Victoria, Australia
- Sydney Institute for Astronomy, School of Physics, The University of Sydney, Sydney, New South Wales, Australia
- CSIRO Space and Astronomy, Epping, New South Wales, Australia
| | | | - James Munday
- Department of Physics, University of Warwick, Coventry, UK
- Isaac Newton Group of Telescopes, Santa Cruz de La Palma, Spain
| | - Paul O'Brien
- School of Physics and Astronomy, University of Leicester, Leicester, UK
| | - Steven G Parsons
- Department of Physics and Astronomy, University of Sheffield, Sheffield, UK
| | | | - David I Sahman
- Department of Physics and Astronomy, University of Sheffield, Sheffield, UK
| | | | | | - Danny Steeghs
- Department of Physics, University of Warwick, Coventry, UK
- ARC Centre of Excellence for Gravitational Wave Discovery (OzGrav), Monash University, Clayton, Victoria, Australia
| | | | - Christina C Thöne
- Astronomical Institute of the Czech Academy of Sciences, Ondřejov, Czechia
| | | | - David Alexander Kann
- Hessian Research Cluster ELEMENTS, Giersch Science Center (GSC), Goethe University Frankfurt, Campus Riedberg, Frankfurt am Main, Germany
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Yang YH, Troja E, O'Connor B, Fryer CL, Im M, Durbak J, Paek GSH, Ricci R, Bom CR, Gillanders JH, Castro-Tirado AJ, Peng ZK, Dichiara S, Ryan G, van Eerten H, Dai ZG, Chang SW, Choi H, De K, Hu Y, Kilpatrick CD, Kutyrev A, Jeong M, Lee CU, Makler M, Navarete F, Pérez-García I. A lanthanide-rich kilonova in the aftermath of a long gamma-ray burst. Nature 2024; 626:742-745. [PMID: 38383623 DOI: 10.1038/s41586-023-06979-5] [Citation(s) in RCA: 2] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/31/2023] [Accepted: 12/14/2023] [Indexed: 02/23/2024]
Abstract
Observationally, kilonovae are astrophysical transients powered by the radioactive decay of nuclei heavier than iron, thought to be synthesized in the merger of two compact objects1-4. Over the first few days, the kilonova evolution is dominated by a large number of radioactive isotopes contributing to the heating rate2,5. On timescales of weeks to months, its behaviour is predicted to differ depending on the ejecta composition and the merger remnant6-8. Previous work has shown that the kilonova associated with gamma-ray burst 230307A is similar to kilonova AT2017gfo (ref. 9), and mid-infrared spectra revealed an emission line at 2.15 micrometres that was attributed to tellurium. Here we report a multi-wavelength analysis, including publicly available James Webb Space Telescope data9 and our own Hubble Space Telescope data, for the same gamma-ray burst. We model its evolution up to two months after the burst and show that, at these late times, the recession of the photospheric radius and the rapidly decaying bolometric luminosity (Lbol ∝ t-2.7±0.4, where t is time) support the recombination of lanthanide-rich ejecta as they cool.
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Affiliation(s)
- Yu-Han Yang
- Department of Physics, University of Rome "Tor Vergata", Rome, Italy.
| | - Eleonora Troja
- Department of Physics, University of Rome "Tor Vergata", Rome, Italy.
- INAF - Istituto Nazionale di Astrofisica, Rome, Italy.
| | - Brendan O'Connor
- Department of Physics, The George Washington University, Washington DC, USA
- Department of Astronomy, University of Maryland, College Park, MD, USA
- Astrophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - Chris L Fryer
- Computer, Computational, and Statistical Sciences Division, Los Alamos National Laboratory, Los Alamos, NM, USA
- Center for Theoretical Astrophysics, Los Alamos National Laboratory, Los Alamos, NM, USA
- The University of Arizona, Tucson, AZ, USA
- Department of Physics and Astronomy, The University of New Mexico, Albuquerque, NM, USA
- The George Washington University, Washington DC, USA
| | - Myungshin Im
- SNU Astronomy Research Center, Astronomy Program, Department of Physics and Astronomy, Seoul National University, Seoul, Republic of Korea
| | - Joe Durbak
- Department of Astronomy, University of Maryland, College Park, MD, USA
- Astrophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - Gregory S H Paek
- SNU Astronomy Research Center, Astronomy Program, Department of Physics and Astronomy, Seoul National University, Seoul, Republic of Korea
| | - Roberto Ricci
- Istituto Nazionale di Ricerca Metrologica, Turin, Italy
- INAF - Istituto di Radioastronomia, Bologna, Italy
| | - Clécio R Bom
- Centro Brasileiro de Pesquisas Físicas, Rio de Janeiro, Brazil
- Centro Federal de Educação Tecnológica Celso Suckow da Fonseca, Rodovia Mário Covas, Itaguaí, Brazil
| | | | - Alberto J Castro-Tirado
- Instituto de Astrofísica de Andalucía (IAA-CSIC), Granada, Spain
- Unidad Asociada al CSIC Departamento de Ingeniería de Sistemas y Automática, Escuela de Ingenierías Industriales, Universidad de Málaga, Málaga, Spain
| | - Zong-Kai Peng
- Institute for Frontier in Astronomy and Astrophysics, Beijing Normal University, Beijing, China
- Department of Astronomy, Beijing Normal University, Beijing, China
| | - Simone Dichiara
- Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA, USA
| | - Geoffrey Ryan
- Perimeter Institute for Theoretical Physics, Waterloo, Ontario, Canada
| | | | - Zi-Gao Dai
- Department of Astronomy, School of Physical Sciences, University of Science and Technology of China, Hefei, China
| | - Seo-Won Chang
- SNU Astronomy Research Center, Astronomy Program, Department of Physics and Astronomy, Seoul National University, Seoul, Republic of Korea
| | - Hyeonho Choi
- SNU Astronomy Research Center, Astronomy Program, Department of Physics and Astronomy, Seoul National University, Seoul, Republic of Korea
| | - Kishalay De
- Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA, USA
| | - Youdong Hu
- Instituto de Astrofísica de Andalucía (IAA-CSIC), Granada, Spain
| | - Charles D Kilpatrick
- Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA) and Department of Physics and Astronomy, Northwestern University, Evanston, IL, USA
| | - Alexander Kutyrev
- Department of Astronomy, University of Maryland, College Park, MD, USA
- Astrophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - Mankeun Jeong
- SNU Astronomy Research Center, Astronomy Program, Department of Physics and Astronomy, Seoul National University, Seoul, Republic of Korea
| | - Chung-Uk Lee
- Korea Astronomy and Space Science Institute, Daejeon, Republic of Korea
| | - Martin Makler
- Centro Brasileiro de Pesquisas Físicas, Rio de Janeiro, Brazil
- International Center for Advanced Studies and Instituto de Ciencias Físicas, ECyT-UNSAM and CONICET, Buenos Aires, Argentina
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65
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Zhu W, Xie Y, Qian Y, Jia J, Zhang L, Wang X. Development and analysis of two-dimensional point-ahead angle mechanism for space gravitational-wave detection. THE REVIEW OF SCIENTIFIC INSTRUMENTS 2024; 95:025002. [PMID: 38350474 DOI: 10.1063/5.0186061] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/03/2023] [Accepted: 01/03/2024] [Indexed: 02/15/2024]
Abstract
To detect low-frequency gravitational waves, it is necessary to eliminate the interference of geo-noise and build a laser interference gravitational-wave detection device in space. Space gravitational-wave detection missions, namely Taiji, LISA, and Tianqin, have been planning to achieve picometer sensitivity on an interferometer arm of several million kilometers to meet the gravitational-wave detection requirements. Because of the orbit evolution and the time delay in interferometer arms, the direction of the transmitted laser beam changes; consequently, a remote telescope cannot receive the laser beam to complete the inter-satellite laser interference. In this study, a two-dimensional point-ahead angle mechanism (2DPAAM) is designed and demonstrated to solve the aforementioned problem. Based on the design concept of aligning the rotation center with the mirror surface center, the 2DPAAM employs a four-link flexible-hinge structure, length expanding and contracting piezoelectric stack actuators, and closed-loop control of capacitive sensors to realize two-dimensional picometer-stable, high-precision rotation. A static model is established to analyze the rotational characteristics, and finite element analysis is performed to study the mechanical properties and to verify the rotational characteristics. The yaw and pitch stiffness errors are ∼0.93% and 5.9%, respectively, when the theoretical results are compared with the simulation results. A series of experiments are conducted on the developed 2DPAAM, and the results show that the rotary ranges of yaw and pitch motions attain ±270 and ±268 µrad, respectively. The rotational accuracies of both yaw and pitch motions attain ∼0.35 µrad, and the optical path difference is less than 10pm/Hz when the frequency is between 1 mHz and 1 Hz, by analogy.
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Affiliation(s)
- Weizhou Zhu
- Key Laboratory of Space Active Opto-electronics Technology, Shanghai Institute of Technical Physics, Chinese Academy of Sciences, Shanghai 200083, China
- School of Electronic, Electrical and Communication Engineering, University of Chinese Academy of Sciences, Beijing 100049, China
| | - Yong Xie
- Key Laboratory of Space Active Opto-electronics Technology, Shanghai Institute of Technical Physics, Chinese Academy of Sciences, Shanghai 200083, China
| | - Yuchen Qian
- Key Laboratory of Space Active Opto-electronics Technology, Shanghai Institute of Technical Physics, Chinese Academy of Sciences, Shanghai 200083, China
- School of Electronic, Electrical and Communication Engineering, University of Chinese Academy of Sciences, Beijing 100049, China
| | - Jianjun Jia
- Key Laboratory of Space Active Opto-electronics Technology, Shanghai Institute of Technical Physics, Chinese Academy of Sciences, Shanghai 200083, China
- School of Electronic, Electrical and Communication Engineering, University of Chinese Academy of Sciences, Beijing 100049, China
| | - Liang Zhang
- Key Laboratory of Space Active Opto-electronics Technology, Shanghai Institute of Technical Physics, Chinese Academy of Sciences, Shanghai 200083, China
- School of Electronic, Electrical and Communication Engineering, University of Chinese Academy of Sciences, Beijing 100049, China
| | - Xue Wang
- Key Laboratory of Space Active Opto-electronics Technology, Shanghai Institute of Technical Physics, Chinese Academy of Sciences, Shanghai 200083, China
- School of Electronic, Electrical and Communication Engineering, University of Chinese Academy of Sciences, Beijing 100049, China
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66
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Hartley D, Käding C, Howl R, Fuentes I. Quantum-enhanced screened dark energy detection. THE EUROPEAN PHYSICAL JOURNAL. C, PARTICLES AND FIELDS 2024; 84:49. [PMID: 38261898 PMCID: PMC10796756 DOI: 10.1140/epjc/s10052-023-12360-7] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 03/21/2023] [Accepted: 12/17/2023] [Indexed: 01/25/2024]
Abstract
We propose an experiment based on a Bose-Einstein condensate interferometer for strongly constraining fifth-force models. Additional scalar fields from modified gravity or higher dimensional theories may account for dark energy and the accelerating expansion of the Universe. These theories have led to proposed screening mechanisms to fit within the tight experimental bounds on fifth-force searches. We show that our proposed experiment would greatly improve the existing constraints on these screening models by many orders of magnitude.
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Affiliation(s)
- Daniel Hartley
- Faculty of Physics, University of Vienna, Boltzmanngasse 5, 1090 Vienna, Austria
| | - Christian Käding
- Technische Universität Wien, Atominstitut, Stadionallee 2, 1020 Vienna, Austria
- National Research University Higher School of Economics, 101000 Moscow, Russia
- School of Physics and Astronomy, University of Nottingham, University Park, Nottingham, NG7 2RD UK
| | - Richard Howl
- Department of Physics, Royal Holloway, University of London, Egham, Surrey, TW20 0EX UK
- Quantum Group, Department of Computer Science, University of Oxford, Wolfson Building, Parks Road, Oxford, OX1 3QD UK
- QICI Quantum Information and Computation Initiative, Department of Computer Science, The University of Hong Kong, Pokfulam Road, Pokfulam, Hong Kong
- School of Mathematical Sciences, University of Nottingham, University Park, Nottingham, NG7 2RD UK
| | - Ivette Fuentes
- School of Mathematical Sciences, University of Nottingham, University Park, Nottingham, NG7 2RD UK
- School of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ UK
- Keble College, Oxford, OX1 3PG UK
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67
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Gefen T, Tarafder R, Adhikari RX, Chen Y. Quantum Precision Limits of Displacement Noise-Free Interferometers. PHYSICAL REVIEW LETTERS 2024; 132:020801. [PMID: 38277601 DOI: 10.1103/physrevlett.132.020801] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/07/2022] [Revised: 07/19/2023] [Accepted: 12/06/2023] [Indexed: 01/28/2024]
Abstract
Current laser-interferometric gravitational wave detectors suffer from a fundamental limit to their precision due to the displacement noise of optical elements contributed by various sources. Several schemes for displacement noise-free interferometers (DFI) have been proposed to mitigate their effects. The idea behind these schemes is similar to decoherence-free subspaces in quantum sensing; i.e., certain modes contain information about the gravitational waves but are insensitive to the mirror motion (displacement noise). We derive quantum precision limits for general DFI schemes, including optimal measurement basis and optimal squeezing schemes. We introduce a triangular cavity DFI scheme and apply our general bounds to it. Precision analysis of this scheme with different noise models shows that the DFI property leads to interesting sensitivity profiles and improved precision due to noise mitigation and larger gain from squeezing.
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Affiliation(s)
- Tuvia Gefen
- Institute for Quantum Information and Matter, California Institute of Technology, Pasadena, California 91125, USA
| | - Rajashik Tarafder
- Theoretical Astrophysics, Walter Burke Institute for Theoretical Physics, California Institute of Technology, Pasadena, California 91125, USA
- LIGO Laboratory, California Institute of Technology, Pasadena, California 91125, USA
| | - Rana X Adhikari
- LIGO Laboratory, California Institute of Technology, Pasadena, California 91125, USA
| | - Yanbei Chen
- Theoretical Astrophysics, Walter Burke Institute for Theoretical Physics, California Institute of Technology, Pasadena, California 91125, USA
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68
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Frost BL. Foundations of the Wentzel-Kramers-Brillouin approximation for models of cochlear mechanics in 1- and 2-D. THE JOURNAL OF THE ACOUSTICAL SOCIETY OF AMERICA 2024; 155:358-379. [PMID: 38236807 PMCID: PMC10800151 DOI: 10.1121/10.0024355] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/20/2023] [Revised: 12/23/2023] [Accepted: 12/27/2023] [Indexed: 01/23/2024]
Abstract
The Wentzel-Kramers-Brillouin (WKB) approximation is frequently used to explore the mechanics of the cochlea. As opposed to numerical strategies, the WKB approximation facilitates analysis of model results through interpretable closed-form equations and can be implemented with relative ease. As a result, it has maintained relevance in the study of cochlear mechanics for half of a century. Over this time, it has been employed to study a variety of phenomena, including the limits of frequency tuning, active displacement amplification within the organ of Corti, feedforward mechanisms in the cochlea, and otoacoustic emissions. Despite this ubiquity, it is challenging to find rigorous exposition of the WKB approximation's formulation, derivation, and implementation in cochlear mechanics literature. In this tutorial, the foundations of the WKB approximation are discussed in application to models of one- and two-dimensional cochlear macromechanics. This includes mathematical background, rigorous derivation and details of its implementation in software.
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Affiliation(s)
- Brian L Frost
- Department of Electrical Engineering, Columbia University, 500 West 120th Street, Mudd 1310, New York, New York 10027, USA
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Chen P, Gal-Yam A, Sollerman J, Schulze S, Post RS, Liu C, Ofek EO, Das KK, Fremling C, Horesh A, Katz B, Kushnir D, Kasliwal MM, Kulkarni SR, Liu D, Liu X, Miller AA, Rose K, Waxman E, Yang S, Yao Y, Zackay B, Bellm EC, Dekany R, Drake AJ, Fang Y, Fynbo JPU, Groom SL, Helou G, Irani I, Jegou du Laz T, Liu X, Mazzali PA, Neill JD, Qin YJ, Riddle RL, Sharon A, Strotjohann NL, Wold A, Yan L. A 12.4-day periodicity in a close binary system after a supernova. Nature 2024; 625:253-258. [PMID: 38200292 DOI: 10.1038/s41586-023-06787-x] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/19/2023] [Accepted: 10/26/2023] [Indexed: 01/12/2024]
Abstract
Neutron stars and stellar-mass black holes are the remnants of massive star explosions1. Most massive stars reside in close binary systems2, and the interplay between the companion star and the newly formed compact object has been theoretically explored3, but signatures for binarity or evidence for the formation of a compact object during a supernova explosion are still lacking. Here we report a stripped-envelope supernova, SN 2022jli, which shows 12.4-day periodic undulations during the declining light curve. Narrow Hα emission is detected in late-time spectra with concordant periodic velocity shifts, probably arising from hydrogen gas stripped from a companion and accreted onto the compact remnant. A new Fermi-LAT γ-ray source is temporally and positionally consistent with SN 2022jli. The observed properties of SN 2022jli, including periodic undulations in the optical light curve, coherent Hα emission shifting and evidence for association with a γ-ray source, point to the explosion of a massive star in a binary system leaving behind a bound compact remnant. Mass accretion from the companion star onto the compact object powers the light curve of the supernova and generates the γ-ray emission.
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Affiliation(s)
- Ping Chen
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel.
| | - Avishay Gal-Yam
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel
| | - Jesper Sollerman
- The Oskar Klein Centre, Department of Astronomy, Stockholm University, Stockholm, Sweden
| | - Steve Schulze
- The Oskar Klein Centre, Department of Physics, Stockholm University, Stockholm, Sweden
| | | | - Chang Liu
- Department of Physics and Astronomy, Northwestern University, Evanston, IL, USA
- Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA), Northwestern University, Evanston, IL, USA
| | - Eran O Ofek
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel
| | - Kaustav K Das
- Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA, USA
| | - Christoffer Fremling
- Caltech Optical Observatories, California Institute of Technology, Pasadena, CA, USA
- Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA, USA
| | - Assaf Horesh
- Racah Institute of Physics, The Hebrew University of Jerusalem, Jerusalem, Israel
| | - Boaz Katz
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel
| | - Doron Kushnir
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel
| | - Mansi M Kasliwal
- Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA, USA
| | - Shri R Kulkarni
- Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA, USA
| | - Dezi Liu
- South-Western Institute for Astronomy Research, Yunnan University, Kunming, Yunnan Province, People's Republic of China
| | - Xiangkun Liu
- South-Western Institute for Astronomy Research, Yunnan University, Kunming, Yunnan Province, People's Republic of China
| | - Adam A Miller
- Department of Physics and Astronomy, Northwestern University, Evanston, IL, USA
- Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA), Northwestern University, Evanston, IL, USA
| | - Kovi Rose
- Sydney Institute for Astronomy, School of Physics, The University of Sydney, Sydney, New South Wales, Australia
| | - Eli Waxman
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel
| | - Sheng Yang
- The Oskar Klein Centre, Department of Astronomy, Stockholm University, Stockholm, Sweden
- Henan Academy of Sciences, Zhengzhou, People's Republic of China
| | - Yuhan Yao
- Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA, USA
| | - Barak Zackay
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel
| | - Eric C Bellm
- DIRAC Institute, Department of Astronomy, University of Washington, Seattle, WA, USA
| | - Richard Dekany
- Caltech Optical Observatories, California Institute of Technology, Pasadena, CA, USA
| | - Andrew J Drake
- Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA, USA
| | - Yuan Fang
- South-Western Institute for Astronomy Research, Yunnan University, Kunming, Yunnan Province, People's Republic of China
| | - Johan P U Fynbo
- The Cosmic DAWN Center, Copenhagen, Denmark
- Niels Bohr Institute, University of Copenhagen, Copenhagen, Denmark
| | - Steven L Groom
- IPAC, California Institute of Technology, Pasadena, CA, USA
| | - George Helou
- IPAC, California Institute of Technology, Pasadena, CA, USA
| | - Ido Irani
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel
| | - Theophile Jegou du Laz
- Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA, USA
| | - Xiaowei Liu
- South-Western Institute for Astronomy Research, Yunnan University, Kunming, Yunnan Province, People's Republic of China
| | - Paolo A Mazzali
- Astrophysics Research Institute, Liverpool John Moores University, Liverpool, UK
- Max-Planck Institute for Astrophysics, Garching, Germany
| | - James D Neill
- Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA, USA
| | - Yu-Jing Qin
- Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA, USA
| | - Reed L Riddle
- Caltech Optical Observatories, California Institute of Technology, Pasadena, CA, USA
| | - Amir Sharon
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel
| | - Nora L Strotjohann
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel
| | - Avery Wold
- IPAC, California Institute of Technology, Pasadena, CA, USA
| | - Lin Yan
- Caltech Optical Observatories, California Institute of Technology, Pasadena, CA, USA
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YAMADA S, NAGAKURA H, AKAHO R, HARADA A, FURUSAWA S, IWAKAMI W, OKAWA H, MATSUFURU H, SUMIYOSHI K. Physical mechanism of core-collapse supernovae that neutrinos drive. PROCEEDINGS OF THE JAPAN ACADEMY. SERIES B, PHYSICAL AND BIOLOGICAL SCIENCES 2024; 100:190-233. [PMID: 38462501 PMCID: PMC11105976 DOI: 10.2183/pjab.100.015] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/05/2023] [Accepted: 12/05/2023] [Indexed: 03/12/2024]
Abstract
The current understanding of the mechanism of core-collapse supernovae (CCSNe), one of the most energetic events in the universe associated with the death of massive stars and the main formation channel of compact objects such as neutron stars and black holes, is reviewed for broad readers from different disciplines of science who may not be familiar with the object. Therefore, we emphasize the physical aspects than the results of individual model simulations, although large-scale high-fidelity simulations have played the most important roles in the progress we have witnessed in the past few decades. It is now believed that neutrinos are the most important agent in producing the commonest type of CCSNe. The so-called neutrino-heating mechanism will be the focus of this review and its crucial ingredients in micro- and macrophysics and in numerics will be explained one by one. We will also try to elucidate the remaining issues.
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Affiliation(s)
- Shoichi YAMADA
- Department of Physics, Faculty of Science and Engineering, Waseda University, Tokyo, Japan
- Research Institute for Science and Engineering, Waseda University, Tokyo, Japan
| | - Hiroki NAGAKURA
- National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan
| | - Ryuichiro AKAHO
- Department of Physics, Faculty of Science and Engineering, Waseda University, Tokyo, Japan
| | - Akira HARADA
- Interdisciplinary Theoretical and Mathematical Sciences Program (iTHEMS), RIKEN, Wako, Saitama, Japan
| | - Shun FURUSAWA
- College of Science and Engineering, Kanto Gakuin University, Yokohama, Kanagawa, Japan
| | - Wakana IWAKAMI
- Department of Physics, Faculty of Science and Engineering, Waseda University, Tokyo, Japan
| | - Hirotada OKAWA
- Waseda Institute for Advanced Study, Waseda University, Tokyo, Japan
| | - Hideo MATSUFURU
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki, Japan
| | - Kohsuke SUMIYOSHI
- National Institute of Technology, Numazu College, Numazu, Shizuoka, Japan
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71
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Zhang J, Liu X, Wang H, Guo J, Yang X, Ren C, Zhou W, Shen D. Near thermal noise limit, 5W single frequency fiber laser base on the ring cavity configuration. OPTICS EXPRESS 2024; 32:104-112. [PMID: 38175041 DOI: 10.1364/oe.507390] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/03/2023] [Accepted: 11/15/2023] [Indexed: 01/05/2024]
Abstract
In this study, we present an ultralow noise single-frequency fiber laser operating at 1550 nm, utilizing a traveling-wave ring cavity configuration. The frequency noise of the laser approaches the thermal noise limit, achieving a white noise level of 0.025 Hz2/Hz, resulting in an instantaneous linewidth of 0.08 Hz. After amplification, the output power reaches 4.94 W while maintaining the same low white noise level as the laser oscillator. The integration linewidths of the laser oscillator and amplifier are 221 Hz and 665 Hz, respectively, with both exhibiting relative intensity noises that approach the quantum shot noise limit. To the best of our knowledge, this work shows the lowest frequency noise combined with relatively high power for this type of ring cavity fiber laser.
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72
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Pang PTH, Dietrich T, Coughlin MW, Bulla M, Tews I, Almualla M, Barna T, Kiendrebeogo RW, Kunert N, Mansingh G, Reed B, Sravan N, Toivonen A, Antier S, VandenBerg RO, Heinzel J, Nedora V, Salehi P, Sharma R, Somasundaram R, Van Den Broeck C. An updated nuclear-physics and multi-messenger astrophysics framework for binary neutron star mergers. Nat Commun 2023; 14:8352. [PMID: 38123551 PMCID: PMC10733434 DOI: 10.1038/s41467-023-43932-6] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/23/2023] [Accepted: 11/24/2023] [Indexed: 12/23/2023] Open
Abstract
The multi-messenger detection of the gravitational-wave signal GW170817, the corresponding kilonova AT2017gfo and the short gamma-ray burst GRB170817A, as well as the observed afterglow has delivered a scientific breakthrough. For an accurate interpretation of all these different messengers, one requires robust theoretical models that describe the emitted gravitational-wave, the electromagnetic emission, and dense matter reliably. In addition, one needs efficient and accurate computational tools to ensure a correct cross-correlation between the models and the observational data. For this purpose, we have developed the Nuclear-physics and Multi-Messenger Astrophysics framework NMMA. The code allows incorporation of nuclear-physics constraints at low densities as well as X-ray and radio observations of isolated neutron stars. In previous works, the NMMA code has allowed us to constrain the equation of state of supranuclear dense matter, to measure the Hubble constant, and to compare dense-matter physics probed in neutron-star mergers and in heavy-ion collisions, and to classify electromagnetic observations and perform model selection. Here, we show an extension of the NMMA code as a first attempt of analyzing the gravitational-wave signal, the kilonova, and the gamma-ray burst afterglow simultaneously. Incorporating all available information, we estimate the radius of a 1.4M⊙ neutron star to be [Formula: see text] km.
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Affiliation(s)
- Peter T H Pang
- Nikhef, Science Park 105, 1098 XG, Amsterdam, The Netherlands
- Institute for Gravitational and Subatomic Physics (GRASP), Utrecht University, Princetonplein 1, 3584 CC, Utrecht, The Netherlands
| | - Tim Dietrich
- Institut für Physik und Astronomie, Universität Potsdam, Haus 28, Karl-Liebknecht-Str. 24/25, 14476, Potsdam, Germany.
- Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Am Mühlenberg 1, 14476, Potsdam, Germany.
| | - Michael W Coughlin
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, 55455, USA
| | - Mattia Bulla
- The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, SE-106 91, Stockholm, Sweden
- Department of Physics and Earth Science, University of Ferrara, Via Saragat 1, I-44122, Ferrara, Italy
- INFN, Sezione di Ferrara, Via Saragat 1, I-44122, Ferrara, Italy
- INAF, Osservatorio Astronomico d'Abruzzo, Via Mentore Maggini snc, 64100, Teramo, Italy
| | - Ingo Tews
- Theoretical Division, Los Alamos National Laboratory, Los Alamos, NM, 87545, USA
| | - Mouza Almualla
- Department of Physics, American University of Sharjah, PO Box 26666, Sharjah, UAE
| | - Tyler Barna
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, 55455, USA
| | - Ramodgwendé Weizmann Kiendrebeogo
- Laboratoire de Physique et de Chimie de l'Environnement, Université Joseph KI-ZERBO, Ouagadougou, Burkina Faso
- Observatoire de la Côte d'Azur, Université Côte d'Azur, CNRS, 96 Boulevard de l'Observatoire, F06304, Nice Cedex 4, France
| | - Nina Kunert
- Institut für Physik und Astronomie, Universität Potsdam, Haus 28, Karl-Liebknecht-Str. 24/25, 14476, Potsdam, Germany
| | - Gargi Mansingh
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, 55455, USA
- Department of Physics, American University, Washington, DC, 20016, USA
| | - Brandon Reed
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, 55455, USA
- Department of Physics and Astronomy, University of Minnesota-Duluth, Duluth, MN, 55812, USA
| | - Niharika Sravan
- Department of Physics, Drexel University, Philadelphia, PA, 19104, USA
| | - Andrew Toivonen
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, 55455, USA
| | - Sarah Antier
- Observatoire de la Côte d'Azur, Université Côte d'Azur, CNRS, 96 Boulevard de l'Observatoire, F06304, Nice Cedex 4, France
| | - Robert O VandenBerg
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, 55455, USA
| | - Jack Heinzel
- Department of Physics, Massachusetts Institute of Technology, 77 Massachusetts Ave, Cambridge, MA, 02139, USA
| | - Vsevolod Nedora
- Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Am Mühlenberg 1, 14476, Potsdam, Germany
| | - Pouyan Salehi
- Institut für Physik und Astronomie, Universität Potsdam, Haus 28, Karl-Liebknecht-Str. 24/25, 14476, Potsdam, Germany
| | - Ritwik Sharma
- Department of Physics, Deshbandhu College, University of Delhi, New Delhi, India
| | - Rahul Somasundaram
- Theoretical Division, Los Alamos National Laboratory, Los Alamos, NM, 87545, USA
- Université Lyon, Université Claude Bernard Lyon 1, CNRS/IN2P3, IP2I Lyon, UMR 5822, F-69622, Villeurbanne, France
- Department of Physics, Syracuse University, Syracuse, NY, 13244, USA
| | - Chris Van Den Broeck
- Nikhef, Science Park 105, 1098 XG, Amsterdam, The Netherlands
- Institute for Gravitational and Subatomic Physics (GRASP), Utrecht University, Princetonplein 1, 3584 CC, Utrecht, The Netherlands
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73
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Jakobsen GU, Mogull G, Plefka J, Sauer B. Dissipative Scattering of Spinning Black Holes at Fourth Post-Minkowskian Order. PHYSICAL REVIEW LETTERS 2023; 131:241402. [PMID: 38181150 DOI: 10.1103/physrevlett.131.241402] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/15/2023] [Accepted: 11/09/2023] [Indexed: 01/07/2024]
Abstract
We compute the radiation reacted momentum impulse Δp_{i}^{μ}, spin kick ΔS_{i}^{μ}, and scattering angle θ between two scattered spinning massive bodies (black holes or neutron stars) using the N=1 supersymmetric worldline quantum field theory formalism up to fourth post-Minkowskian (4PM) order. Our calculation confirms the state-of-the-art nonspinning results, and extends them to include spin-orbit effects. Advanced multiloop Feynman integral technology including differential equations and the method of regions are applied and extended to deal with the retarded propagators arising in a causal description of the scattering dynamics. From these results we determine a complete set of radiative fluxes at subleading PM order: the 4PM radiated four-momentum and, via linear response, the 3PM radiated angular momentum, both again including spin-orbit effects.
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Affiliation(s)
- Gustav Uhre Jakobsen
- Institut für Physik und IRIS Adlershof, Humboldt Universität zu Berlin, Zum Großen Windkanal 2, 12489 Berlin, Germany
- Max Planck Institut für Gravitationsphysik (Albert Einstein Institut), Am Mühlenberg 1, 14476 Potsdam, Germany
| | - Gustav Mogull
- Institut für Physik und IRIS Adlershof, Humboldt Universität zu Berlin, Zum Großen Windkanal 2, 12489 Berlin, Germany
- Max Planck Institut für Gravitationsphysik (Albert Einstein Institut), Am Mühlenberg 1, 14476 Potsdam, Germany
| | - Jan Plefka
- Institut für Physik und IRIS Adlershof, Humboldt Universität zu Berlin, Zum Großen Windkanal 2, 12489 Berlin, Germany
| | - Benjamin Sauer
- Institut für Physik und IRIS Adlershof, Humboldt Universität zu Berlin, Zum Großen Windkanal 2, 12489 Berlin, Germany
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74
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Combi L, Siegel DM. Jets from Neutron-Star Merger Remnants and Massive Blue Kilonovae. PHYSICAL REVIEW LETTERS 2023; 131:231402. [PMID: 38134805 DOI: 10.1103/physrevlett.131.231402] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 03/11/2023] [Revised: 09/27/2023] [Accepted: 11/14/2023] [Indexed: 12/24/2023]
Abstract
We perform three-dimensional general-relativistic magnetohydrodynamic simulations with weak interactions of binary neutron-star (BNS) mergers resulting in a long-lived remnant neutron star, with properties typical of galactic BNS and consistent with those inferred for the first observed BNS merger GW170817. We demonstrate self-consistently that within ≲30 ms postmerger magnetized (σ∼5-10) incipient jets emerge with asymptotic Lorentz factor Γ∼5-10, which successfully break out from the merger debris within ≲20 ms. A fast (v≲0.6c), magnetized (σ∼0.1) wind surrounds the jet core and generates a UV/blue kilonova precursor on timescales of hours, similar to the precursor signal due to free neutron decay in fast dynamical ejecta. Postmerger ejecta are quickly dominated by magnetohydrodynamically driven outflows from an accretion disk. We demonstrate that, within only 50 ms postmerger, ≳2×10^{-2}M_{⊙} of lanthanide-free, quasispherical ejecta with velocities ∼0.1-0.2c is launched, yielding a kilonova signal consistent with GW170817 on timescales of ≲5 d.
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Affiliation(s)
- Luciano Combi
- Perimeter Institute for Theoretical Physics, Waterloo, Ontario N2L 2Y5, Canada
- Department of Physics, University of Guelph, Guelph, Ontario N1G 2W1, Canada
- Instituto Argentino de Radioastronomía (IAR, CCT La Plata, CONICET/CIC), C.C.5, (1984) Villa Elisa, Buenos Aires, Argentina
| | - Daniel M Siegel
- Perimeter Institute for Theoretical Physics, Waterloo, Ontario N2L 2Y5, Canada
- Department of Physics, University of Guelph, Guelph, Ontario N1G 2W1, Canada
- Institute of Physics, University of Greifswald, D-17489 Greifswald, Germany
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75
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Oppenheim J, Sparaciari C, Šoda B, Weller-Davies Z. Gravitationally induced decoherence vs space-time diffusion: testing the quantum nature of gravity. Nat Commun 2023; 14:7910. [PMID: 38049417 PMCID: PMC10696068 DOI: 10.1038/s41467-023-43348-2] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/12/2023] [Accepted: 11/08/2023] [Indexed: 12/06/2023] Open
Abstract
We consider two interacting systems when one is treated classically while the other system remains quantum. Consistent dynamics of this coupling has been shown to exist, and explored in the context of treating space-time classically. Here, we prove that any such hybrid dynamics necessarily results in decoherence of the quantum system, and a breakdown in predictability in the classical phase space. We further prove that a trade-off between the rate of this decoherence and the degree of diffusion induced in the classical system is a general feature of all classical quantum dynamics; long coherence times require strong diffusion in phase-space relative to the strength of the coupling. Applying the trade-off relation to gravity, we find a relationship between the strength of gravitationally-induced decoherence versus diffusion of the metric and its conjugate momenta. This provides an experimental signature of theories in which gravity is fundamentally classical. Bounds on decoherence rates arising from current interferometry experiments, combined with precision measurements of mass, place significant restrictions on theories where Einstein's classical theory of gravity interacts with quantum matter. We find that part of the parameter space of such theories are already squeezed out, and provide figures of merit which can be used in future mass measurements and interference experiments.
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Affiliation(s)
- Jonathan Oppenheim
- Department of Physics and Astronomy, University College London, Gower Street, London, WC1E 6BT, UK.
| | - Carlo Sparaciari
- Department of Physics and Astronomy, University College London, Gower Street, London, WC1E 6BT, UK
| | - Barbara Šoda
- Department of Physics and Astronomy, University College London, Gower Street, London, WC1E 6BT, UK
- Department of Physics, University of Waterloo, Waterloo, ON, Canada
- Perimeter Institute for Theoretical Physics, Waterloo, ON, Canada
| | - Zachary Weller-Davies
- Department of Physics and Astronomy, University College London, Gower Street, London, WC1E 6BT, UK
- Perimeter Institute for Theoretical Physics, Waterloo, ON, Canada
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76
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Poli E, Bland T, White SJM, Mark MJ, Ferlaino F, Trabucco S, Mannarelli M. Glitches in Rotating Supersolids. PHYSICAL REVIEW LETTERS 2023; 131:223401. [PMID: 38101354 DOI: 10.1103/physrevlett.131.223401] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/16/2023] [Revised: 09/11/2023] [Accepted: 10/20/2023] [Indexed: 12/17/2023]
Abstract
Glitches, spin-up events in neutron stars, are of prime interest, as they reveal properties of nuclear matter at subnuclear densities. We numerically investigate the glitch mechanism due to vortex unpinning using analogies between neutron stars and dipolar supersolids. We explore the vortex and crystal dynamics during a glitch and its dependence on the supersolid quality, providing a tool to study glitches from different radial depths of a neutron star. Benchmarking our theory against neutron-star observations, our work will open a new avenue for the quantum simulation of stellar objects from Earth.
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Affiliation(s)
- Elena Poli
- Universität Innsbruck, Fakultät für Mathematik, Informatik und Physik, Institut für Experimentalphysik, 6020 Innsbruck, Austria
| | - Thomas Bland
- Universität Innsbruck, Fakultät für Mathematik, Informatik und Physik, Institut für Experimentalphysik, 6020 Innsbruck, Austria
| | - Samuel J M White
- Universität Innsbruck, Fakultät für Mathematik, Informatik und Physik, Institut für Experimentalphysik, 6020 Innsbruck, Austria
- Institut für Quantenoptik und Quanteninformation, Österreichische Akademie der Wissenschaften, 6020 Innsbruck, Austria
| | - Manfred J Mark
- Universität Innsbruck, Fakultät für Mathematik, Informatik und Physik, Institut für Experimentalphysik, 6020 Innsbruck, Austria
- Institut für Quantenoptik und Quanteninformation, Österreichische Akademie der Wissenschaften, 6020 Innsbruck, Austria
| | - Francesca Ferlaino
- Universität Innsbruck, Fakultät für Mathematik, Informatik und Physik, Institut für Experimentalphysik, 6020 Innsbruck, Austria
- Institut für Quantenoptik und Quanteninformation, Österreichische Akademie der Wissenschaften, 6020 Innsbruck, Austria
| | - Silvia Trabucco
- INFN Laboratori Nazionali del Gran Sasso, 67100 Assergi (AQ), Italy
- Gran Sasso Science Institute, 67100 L'Aquila, Italy
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77
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Yu XD, Tong DM. Evolution Operator Can Always Be Separated into the Product of Holonomy and Dynamic Operators. PHYSICAL REVIEW LETTERS 2023; 131:200202. [PMID: 38039483 DOI: 10.1103/physrevlett.131.200202] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/01/2023] [Revised: 09/25/2023] [Accepted: 10/20/2023] [Indexed: 12/03/2023]
Abstract
The geometric phase is a fundamental quantity characterizing the holonomic feature of quantum systems. It is well known that the evolution operator of a quantum system undergoing a cyclic evolution can be simply written as the product of holonomic and dynamical components for the three special cases concerning the Berry phase, adiabatic non-Abelian geometric phase, and nonadiabatic Abelian geometric phase. However, for the most general case concerning the nonadiabatic non-Abelian geometric phase, how to separate the evolution operator into holonomic and dynamical components is a long-standing open problem. In this Letter, we solve this open problem. We show that the evolution operator of a quantum system can always be separated into the product of holonomy and dynamic operators. Based on it, we further derive a matrix representation of this separation formula for cyclic evolution, and give a necessary and sufficient condition for a general evolution being purely holonomic. Our finding is not only of theoretical interest itself, but also of vital importance for the application of quantum holonomy. It unifies the representations of all four types of evolution concerning the adiabatic/nonadiabatic Abelian/non-Abelian geometric phase, and provides a general approach to realizing purely holonomic evolution.
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Affiliation(s)
- Xiao-Dong Yu
- Department of Physics, Shandong University, Jinan 250100, China
| | - D M Tong
- Department of Physics, Shandong University, Jinan 250100, China
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78
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Zhao M, Tao Y, Weber K, Kaune T, Schuster S, Hao Z, Wanner G. Method Comparison for Simulating Non-Gaussian Beams and Diffraction for Precision Interferometry. SENSORS (BASEL, SWITZERLAND) 2023; 23:9024. [PMID: 38005412 PMCID: PMC10674269 DOI: 10.3390/s23229024] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/09/2023] [Revised: 10/20/2023] [Accepted: 10/21/2023] [Indexed: 11/26/2023]
Abstract
In the context of simulating precision laser interferometers, we use several examples to compare two wavefront decomposition methods-the Mode Expansion Method (MEM) and the Gaussian Beam Decomposition (GBD) method-for their precision and applicability. To assess the performance of these methods, we define different types of errors and study their properties. We specify how the two methods can be fairly compared and based on that, compare the quality of the MEM and GBD through several examples. Here, we test cases for which analytic results are available, i.e., non-clipped circular and general astigmatic Gaussian beams, as well as clipped circular Gaussian beams, in the near, far, and extremely far fields of millions of kilometers occurring in space-gravitational wave detectors. Additionally, we compare the methods for aberrated wavefronts and their interaction with optical components by testing reflections from differently curved mirrors. We find that both methods can generally be used for decomposing non-Gaussian beams. However, which method is more accurate depends on the optical system and simulation settings. In the given examples, the MEM more accurately describes non-clipped Gaussian beams, whereas for clipped Gaussian beams and the interaction with surfaces, the GBD is more precise.
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Grants
- National Key R&D Program of China National Key R&D Program of China
- M.IF.A.QOP18098, CAS's Strategic Pioneer Program on Space Science XDA1502110201 the Chinese Academy of Sciences (CAS) and the Max Planck Society (MPG) in the framework of the LEGACY cooperation on low-frequency gravitational wave astronomy
- FKZ 50OQ1801, EXC 2123, Project ID 390837967 the German Space Agency, DLR and support 1044 by the Federal Ministry for Economic Affairs and Energy based on a resolution of the German 1045 Bundestag (FKZ 50OQ1801) as well as the Deutsche Forschungsgemeinschaft (DFG) funding the 1046 Cluster of Excell
- Project-ID 434617780 the Collaborative Research Centres CRC 1128: geo-Q - Relativistic Geodesy and Gravimetry with Quantum Sensors, project A05 and all work contributions to this paper made by Sönke Schuster, as well as CRC 1464: TerraQ - Relativistic and Quantum-based Geodes
- EXC 2122, Project ID 390833453, EXC 2123, Project ID 390837967 DFG for funding the Clusters of Excellence PhoenixD (EXC 2122, Project ID 390833453) and QuantumFrontiers (EXC 2123, Project ID 390837967) which offer an excellent scientific exchange on optical simulations
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Affiliation(s)
- Mengyuan Zhao
- Key Laboratory of Electronics and Information Technology for Space System, National Space Science Center, Chinese Academy of Sciences, No.1 Nanertiao, Zhongguancun, Haidian District, Beijing 100190, China
- University of Chinese Academy of Sciences, No.19(A) Yuquan Road, Shijingshan District, Beijing 100049, China
- Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Callinstr. 38, 30167 Hannover, Germany;
| | - Yazheng Tao
- University of Chinese Academy of Sciences, No.19(A) Yuquan Road, Shijingshan District, Beijing 100049, China
- School of Fundamental Physics and Mathematical Sciences, Hangzhou Institute for Advanced Study, UCAS, Hangzhou 310024, China (Z.H.)
- TaiJi Laboratory for Gravitational Wave Universe (Beijing/Hangzhou), University of Chinese Academy of Sciences, Beijing 100049, China
| | - Kevin Weber
- Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Callinstr. 38, 30167 Hannover, Germany;
- Institute for Gravitational Physics, Leibniz Universität Hannover, Callinstr. 38, 30167 Hannover, Germany; (K.W.); (S.S.)
| | - Tim Kaune
- Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Callinstr. 38, 30167 Hannover, Germany;
- Institute for Gravitational Physics, Leibniz Universität Hannover, Callinstr. 38, 30167 Hannover, Germany; (K.W.); (S.S.)
| | - Sönke Schuster
- Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Callinstr. 38, 30167 Hannover, Germany;
- Institute for Gravitational Physics, Leibniz Universität Hannover, Callinstr. 38, 30167 Hannover, Germany; (K.W.); (S.S.)
| | - Zhenxiang Hao
- University of Chinese Academy of Sciences, No.19(A) Yuquan Road, Shijingshan District, Beijing 100049, China
- School of Fundamental Physics and Mathematical Sciences, Hangzhou Institute for Advanced Study, UCAS, Hangzhou 310024, China (Z.H.)
- TaiJi Laboratory for Gravitational Wave Universe (Beijing/Hangzhou), University of Chinese Academy of Sciences, Beijing 100049, China
| | - Gudrun Wanner
- Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Callinstr. 38, 30167 Hannover, Germany;
- Institute for Gravitational Physics, Leibniz Universität Hannover, Callinstr. 38, 30167 Hannover, Germany; (K.W.); (S.S.)
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79
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Baumgarte TW, Brügmann B, Cors D, Gundlach C, Hilditch D, Khirnov A, Ledvinka T, Renkhoff S, Fernández IS. Critical Phenomena in the Collapse of Gravitational Waves. PHYSICAL REVIEW LETTERS 2023; 131:181401. [PMID: 37977635 DOI: 10.1103/physrevlett.131.181401] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/26/2023] [Revised: 09/04/2023] [Accepted: 09/22/2023] [Indexed: 11/19/2023]
Abstract
Fine-tuning generic but smooth spherically symmetric initial data for general relativity to the threshold of dynamical black hole formation creates arbitrarily large curvatures, mediated by a universal self-similar solution that acts as an intermediate attractor. For vacuum gravitational waves, however, these critical phenomena have been elusive. We present, for the first time, excellent agreement among three independent numerical simulations of this collapse. Surprisingly, we find no universality, and observe approximate self-similarity for some families of initial data but not for others.
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Affiliation(s)
- Thomas W Baumgarte
- Department of Physics and Astronomy, Bowdoin College, Brunswick, Maine 04011, USA
| | - Bernd Brügmann
- Friedrich-Schiller-Universität, Jena, 07743 Jena, Germany
| | - Daniela Cors
- Friedrich-Schiller-Universität, Jena, 07743 Jena, Germany
| | - Carsten Gundlach
- School of Mathematical Sciences, University of Southampton, Southampton SO17 1BJ, United Kingdom
| | - David Hilditch
- Centro de Astrofísica e Gravitação-CENTRA, Departamento de Física, Instituto Superior Técnico-IST, Universidade de Lisboa-UL, Avenida Rovisco Pais 1, 1049-001 Lisboa, Portugal
| | - Anton Khirnov
- Institute of Theoretical Physics, Faculty of Mathematics and Physics, Charles University, CZ-180 00 Prague, Czech Republic
| | - Tomáš Ledvinka
- Institute of Theoretical Physics, Faculty of Mathematics and Physics, Charles University, CZ-180 00 Prague, Czech Republic
| | - Sarah Renkhoff
- Friedrich-Schiller-Universität, Jena, 07743 Jena, Germany
| | - Isabel Suárez Fernández
- Departament de Física, Universitat de les Illes Balears, IAC3-IEEC, Carretera Valldemossa km 7.5, E-07122 Palma, Spain
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80
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Davis ED. Oklo natural fission reactors and dynamical models of dark energy. RADIATION PROTECTION DOSIMETRY 2023; 199:2288-2292. [PMID: 37934985 DOI: 10.1093/rpd/ncad020] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/16/2022] [Revised: 11/16/2022] [Accepted: 01/12/2023] [Indexed: 11/09/2023]
Abstract
Bounds on the cosmological variation of the fine structure constant α inferred from Oklo neutron capture data are sometimes taken cum grano salis. It is possible to quantify uncertainties related to the treatment of excitation, deformation and the Coulomb interaction. On the basis of this analysis, it is concluded that Oklo data imply the relative change in α over the last 1.9 billion years is < 0.01 ppm (95% CL). Accommodation of this constraint represents a challenge to dark energy models that predict that fundamental constants do change.
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Affiliation(s)
- E D Davis
- Department of Physical and Earth Sciences, Sol Plaatje University, Kimberley NC 8301, South Africa
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81
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Jain M, Amin MA, Pu H. Integrator for general spin-s Gross-Pitaevskii systems. Phys Rev E 2023; 108:055305. [PMID: 38115448 DOI: 10.1103/physreve.108.055305] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/13/2023] [Accepted: 10/13/2023] [Indexed: 12/21/2023]
Abstract
We provide an algorithm, i-SPin 2, for evolving general spin-s Gross-Pitaevskii or nonlinear Schrödinger systems carrying a variety of interactions, where the 2s+1 components of the "spinor" field represent the different spin-multiplicity states. We consider many nonrelativistic interactions up to quartic order in the Schrödinger field (both short and long range, and spin-dependent and spin-independent interactions), including explicit spin-orbit couplings. The algorithm allows for spatially varying external and/or self-generated vector potentials that couple to the spin density of the field. Our work can be used for scenarios ranging from laboratory systems such as spinor Bose-Einstein condensates (BECs), to cosmological or astrophysical systems such as self-interacting bosonic dark matter. As examples, we provide results for two different setups of spin-1 BECs that employ a varying magnetic field and spin-orbit coupling, respectively, and also collisions of spin-1 solitons in dark matter. Our symplectic algorithm is second-order accurate in time, and is extensible to the known higher-order-accurate methods.
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Affiliation(s)
- Mudit Jain
- Department of Physics and Astronomy, Rice University, Houston, Texas 77005, USA
| | - Mustafa A Amin
- Department of Physics and Astronomy, Rice University, Houston, Texas 77005, USA
| | - Han Pu
- Department of Physics and Astronomy, Rice University, Houston, Texas 77005, USA
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82
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Strubbe F. Nonlocality, Superposition, and Time in the 4+1 Formalism. ENTROPY (BASEL, SWITZERLAND) 2023; 25:1493. [PMID: 37998184 PMCID: PMC10670268 DOI: 10.3390/e25111493] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/04/2023] [Revised: 10/14/2023] [Accepted: 10/27/2023] [Indexed: 11/25/2023]
Abstract
The field of quantum gravity struggles with several problems related to time, quantum measurement, nonlocality, and realism. To address these issues, this study develops a 4+1 formalism featuring a flat 4D spacetime evolving with a second form of time, τ, worldlines that locally conserve momentum, and a hypersurface representing the present. As a function of τ, worldlines can spatially readjust and influences can travel backward or forward in the time dimension along these worldlines, offering a physical mechanism for retrocausality. Three theoretical models are presented, elucidating how nonlocality in an EPR experiment, the arrival time problem, and superposition in a Mach-Zehnder interferometer can be understood within this 4+1 framework. These results demonstrate that essential quantum phenomena can be reproduced in the 4+1 formalism while upholding the principles of realism, locality, and determinism at a fundamental level. Additionally, there is no measurement or collapse problem, and a natural explanation for the quantum-to-classical transition is obtained. Furthermore, observations of a 4D block universe and of the flow of time can be simultaneously understood. With these properties, the presented 4+1 formalism lays an interesting foundation for a quantum gravity theory based on intuitive principles and compatible with our observation of time.
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Affiliation(s)
- Filip Strubbe
- Department of Electronics and Information Systems, Ghent University, Tech Lane Ghent Science Park-Campus A 126, 9052 Ghent, Belgium
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83
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Gouttenoire Y. First-Order Phase Transition Interpretation of Pulsar Timing Array Signal Is Consistent with Solar-Mass Black Holes. PHYSICAL REVIEW LETTERS 2023; 131:171404. [PMID: 37955485 DOI: 10.1103/physrevlett.131.171404] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/12/2023] [Accepted: 09/08/2023] [Indexed: 11/14/2023]
Abstract
We perform a Bayesian analysis of NANOGrav 15-yr and IPTA DR2 pulsar timing residuals and show that the recently detected stochastic gravitational-wave background is compatible with a stochastic gravitational-wave background produced by bubble dynamics during a cosmological first-order phase transition. The timing data suggest that the phase transition would occur around QCD confinement temperature and would have a slow rate of completion. This scenario can naturally lead to the abundant production of primordial black holes with solar masses. These primordial black holes can potentially be detected by current and advanced gravitational-wave detectors LIGO-Virgo-Kagra, Einstein Telescope, Cosmic Explorer, by astrometry with GAIA, and by 21-cm survey.
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Affiliation(s)
- Yann Gouttenoire
- School of Physics and Astronomy, Tel-Aviv University, Tel-Aviv 69978, Israel
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84
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Zheng Y, Kouvatsos N, Golomb J, Cavaglià M, Renzini AI, Sakellariadou M. Angular Power Spectrum of Gravitational-Wave Transient Sources as a Probe of the Large-Scale Structure. PHYSICAL REVIEW LETTERS 2023; 131:171403. [PMID: 37955493 DOI: 10.1103/physrevlett.131.171403] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/05/2023] [Accepted: 10/06/2023] [Indexed: 11/14/2023]
Abstract
We present a new, simulation-based inference method to compute the angular power spectrum of the distribution of foreground gravitational-wave transient events. As a first application of this method, we use the binary black hole mergers observed during the LIGO, Virgo, and KAGRA third observation run to test the spatial distribution of these sources. We find no evidence for anisotropy in their angular distribution. We discuss further applications of this method to investigate other gravitational-wave source populations and their correlations to the cosmological large-scale structure.
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Affiliation(s)
- Yanyan Zheng
- Institute of Multi-messenger Astrophysics and Cosmology, Missouri University of Science and Technology, Physics Building, 1315 North Pine Street, Rolla, Missouri 65409, USA
| | - Nikolaos Kouvatsos
- Theoretical Particle Physics and Cosmology Group, Physics Department, King's College London, University of London, Strand, London WC2R 2LS, United Kingdom
| | - Jacob Golomb
- LIGO Laboratory, California Institute of Technology, Pasadena, California 91125, USA
- Department of Physics, California Institute of Technology, Pasadena, California 91125, USA
| | - Marco Cavaglià
- Institute of Multi-messenger Astrophysics and Cosmology, Missouri University of Science and Technology, Physics Building, 1315 North Pine Street, Rolla, Missouri 65409, USA
| | - Arianna I Renzini
- LIGO Laboratory, California Institute of Technology, Pasadena, California 91125, USA
- Department of Physics, California Institute of Technology, Pasadena, California 91125, USA
| | - Mairi Sakellariadou
- Theoretical Particle Physics and Cosmology Group, Physics Department, King's College London, University of London, Strand, London WC2R 2LS, United Kingdom
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85
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Liccardo V, Lenzi CH, Marinho RM, Aguiar OD, Frajuca C, da Silva Bortoli F, Costa CA. The design strain sensitivity of the schenberg spherical resonant antenna for gravitational waves. Sci Rep 2023; 13:17706. [PMID: 37848454 PMCID: PMC10582151 DOI: 10.1038/s41598-023-43808-1] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/17/2023] [Accepted: 09/28/2023] [Indexed: 10/19/2023] Open
Abstract
The main purpose of this study is to review the Schenberg resonant antenna transfer function and to recalculate the antenna design strain sensitivity for gravitational waves. We consider the spherical antenna with six transducers in the semi dodecahedral configuration. When coupled to the antenna, the transducer-sphere system will work as a mass-spring system with three masses. The first one is the antenna effective mass for each quadrupole mode, the second one is the mass of the mechanical structure of the transducer first mechanical mode and the third one is the effective mass of the transducer membrane that makes one of the transducer microwave cavity walls. All the calculations are done for the degenerate (all the sphere quadrupole mode frequencies equal) and non-degenerate sphere cases. We have come to the conclusion that the "ultimate" sensitivity of an advanced version of Schenberg antenna (aSchenberg) is around the standard quantum limit (although the parametric transducers used could, in principle, surpass this limit). However, this sensitivity, in the frequency range where Schenberg operates, has already been achieved by the two aLIGOs in the O3 run, therefore, the only reasonable justification for remounting the Schenberg antenna and trying to place it in the sensitivity of the standard quantum limit would be to detect gravitational waves with another physical principle, different from the one used by laser interferometers. This other physical principle would be the absorption of the gravitational wave energy by a resonant mass like Schenberg.
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Affiliation(s)
- V Liccardo
- Instituto Nacional de Pesquisas Espaciais, São José dos Campos, São Paulo, 12227-010, Brazil.
| | - C H Lenzi
- Instituto Tecnológico de Aeronáutica, São José dos Campos, São Paulo, 12228-900, Brazil
| | - R M Marinho
- Instituto Tecnológico de Aeronáutica, São José dos Campos, São Paulo, 12228-900, Brazil
| | - O D Aguiar
- Instituto Nacional de Pesquisas Espaciais, São José dos Campos, São Paulo, 12227-010, Brazil
| | - C Frajuca
- Universidade Federal do Rio Grande, Rio Grande, Rio Grande do Sul, 96203-900, Brazil
| | | | - C A Costa
- Instituto Nacional de Pesquisas Espaciais, São José dos Campos, São Paulo, 12227-010, Brazil
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86
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Jakobsen GU, Mogull G, Plefka J, Sauer B, Xu Y. Conservative Scattering of Spinning Black Holes at Fourth Post-Minkowskian Order. PHYSICAL REVIEW LETTERS 2023; 131:151401. [PMID: 37897767 DOI: 10.1103/physrevlett.131.151401] [Citation(s) in RCA: 1] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/26/2023] [Accepted: 09/18/2023] [Indexed: 10/30/2023]
Abstract
Using the N=1 supersymmetric, spinning worldline quantum field theory formalism, we compute the conservative spin-orbit part of the momentum impulse Δp_{i}^{μ}, spin kick ΔS_{i}^{μ}, and scattering angle θ from the scattering of two spinning massive bodies (black holes or neutron stars) up to fourth post-Minkowskian (PM) order. These three-loop results extend the state of the art for generically spinning binaries from 3PM to 4PM. They are obtained by employing recursion relations for the integrand construction and advanced multiloop Feynman integral technology in the causal (in-in) worldline quantum field theory framework to directly produce classical observables. We focus on the conservative contribution (including tail effects) and outline the computations for the dissipative contributions as well. Our spin-orbit results agree with next-to-next-to-next-to-leading-order post-Newtonian and test-body data in the respective limits. We also reconfirm the conservative 4PM nonspinning results.
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Affiliation(s)
- Gustav Uhre Jakobsen
- Institut für Physik und IRIS Adlershof, Humboldt Universität zu Berlin, Zum Großen Windkanal 2, 12489 Berlin, Germany
- Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Am Mühlenberg 1, 14476 Potsdam, Germany
| | - Gustav Mogull
- Institut für Physik und IRIS Adlershof, Humboldt Universität zu Berlin, Zum Großen Windkanal 2, 12489 Berlin, Germany
- Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Am Mühlenberg 1, 14476 Potsdam, Germany
| | - Jan Plefka
- Institut für Physik und IRIS Adlershof, Humboldt Universität zu Berlin, Zum Großen Windkanal 2, 12489 Berlin, Germany
| | - Benjamin Sauer
- Institut für Physik und IRIS Adlershof, Humboldt Universität zu Berlin, Zum Großen Windkanal 2, 12489 Berlin, Germany
| | - Yingxuan Xu
- Institut für Physik, Humboldt Universität zu Berlin, Newtonstraße 15, 12489 Berlin, Germany
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87
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Jia J, Novikov V, Brasil TB, Zeuthen E, Müller JH, Polzik ES. Acoustic frequency atomic spin oscillator in the quantum regime. Nat Commun 2023; 14:6396. [PMID: 37828042 PMCID: PMC10570288 DOI: 10.1038/s41467-023-42059-y] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 03/16/2023] [Accepted: 09/28/2023] [Indexed: 10/14/2023] Open
Abstract
Quantum noise reduction and entanglement-enhanced sensing in the acoustic frequency range is an outstanding challenge relevant for a number of applications including magnetometry and broadband noise reduction in gravitational wave detectors. Here we experimentally demonstrate quantum behavior of a macroscopic atomic spin oscillator in the acoustic frequency range. Quantum back-action of the spin measurement, ponderomotive squeezing of light, and virtual spring softening are observed at oscillation frequencies down to the sub-kHz range. Quantum noise sources characteristic of spin oscillators operating in the near-DC frequency range are identified and means for their mitigation are presented.
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Affiliation(s)
- Jun Jia
- Niels Bohr Institute, University of Copenhagen, Copenhagen, Denmark
| | - Valeriy Novikov
- Niels Bohr Institute, University of Copenhagen, Copenhagen, Denmark
- Russian Quantum Center, Skolkovo, Moscow, Russia
| | | | - Emil Zeuthen
- Niels Bohr Institute, University of Copenhagen, Copenhagen, Denmark
| | | | - Eugene S Polzik
- Niels Bohr Institute, University of Copenhagen, Copenhagen, Denmark.
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88
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Trachenko K. Viscosity and diffusion in life processes and tuning of fundamental constants. REPORTS ON PROGRESS IN PHYSICS. PHYSICAL SOCIETY (GREAT BRITAIN) 2023; 86:112601. [PMID: 37811635 DOI: 10.1088/1361-6633/acfd3e] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/28/2023] [Accepted: 09/26/2023] [Indexed: 10/10/2023]
Abstract
Viewed as one of the grandest questions in modern science, understanding fundamental physical constants has been discussed in high-energy particle physics, astronomy and cosmology. Here, I review how condensed matter and liquid physics gives new insights into fundamental constants and their tuning. This is based on two observations: first, cellular life and the existence of observers depend on viscosity and diffusion. Second, the lower bound on viscosity and upper bound on diffusion are set by fundamental constants, and I briefly review this result and related recent developments in liquid physics. I will subsequently show that bounds on viscosity, diffusion and the newly introduced fundamental velocity gradient in a biochemical machine can all be varied while keeping the fine-structure constant and the proton-to-electron mass ratio intact. This implies that it is possible to produce heavy elements in stars but have a viscous planet where all liquids have very high viscosity (for example that of tar or higher) and where life may not exist. Knowing the range of bio-friendly viscosity and diffusion, we will be able to calculate the range of fundamental constants which favour cellular life and observers and compare this tuning with that discussed in high-energy physics previously. This invites an inter-disciplinary research between condensed matter physics and life sciences, and I formulate several questions that life science can address. I finish with a conjecture of multiple tuning and an evolutionary mechanism.
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Affiliation(s)
- K Trachenko
- School of Physical and Chemical Sciences, Queen Mary University of London, Mile End Road, London E1 4NS, United Kingdom
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89
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Goodwin-Jones AW, Zhu H, Blair C, Brown DD, van Heijningen J, Ju L, Zhao C. Single and coupled cavity mode sensing schemes using a diagnostic field. OPTICS EXPRESS 2023; 31:35068-35085. [PMID: 37859247 DOI: 10.1364/oe.502911] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 08/08/2023] [Accepted: 09/13/2023] [Indexed: 10/21/2023]
Abstract
Precise optical mode matching is of critical importance in experiments using squeezed-vacuum states. Automatic spatial-mode matching schemes have the potential to reduce losses and improve loss stability. However, in quantum-enhanced coupled-cavity experiments, such as gravitational-wave detectors, one must also ensure that the sub-cavities are also mode matched. We propose what we believe to be a new mode sensing scheme, which works for simple and coupled cavities. The scheme requires no moving parts, nor tuning of Gouy phases. Instead a diagnostic field tuned to the HG20/LG10 mode frequency is used. The error signals are derived to be proportional to the difference in waist position, and difference in Rayleigh ranges, between the sub-cavity eigenmodes. The two error signals are separable by 90 degrees of demodulation phase. We demonstrate reasonable error signals for a simplified Einstein Telescope optical design. This work will facilitate routine use of extremely high levels of squeezing in current and future gravitational-wave detectors.
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90
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Korobko M, Südbeck J, Steinlechner S, Schnabel R. Mitigating Quantum Decoherence in Force Sensors by Internal Squeezing. PHYSICAL REVIEW LETTERS 2023; 131:143603. [PMID: 37862640 DOI: 10.1103/physrevlett.131.143603] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 03/20/2023] [Accepted: 09/07/2023] [Indexed: 10/22/2023]
Abstract
The most efficient approach to laser interferometric force sensing to date uses monochromatic carrier light with its signal sideband spectrum in a squeezed vacuum state. Quantum decoherence, i.e., mixing with an ordinary vacuum state due to optical losses, is the main sensitivity limit. In this Letter, we present both theoretical and experimental evidence that quantum decoherence in high-precision laser interferometric force sensors enhanced with optical cavities and squeezed light injection can be mitigated by a quantum squeeze operation inside the sensor's cavity. Our experiment shows an enhanced measurement sensitivity that is independent of the optical readout loss in a wide range. Our results pave the way for quantum improvements in scenarios where high decoherence previously precluded the use of squeezed light. Our results hold significant potential for advancing the field of quantum sensors and enabling new experimental approaches in high-precision measurement technology.
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Affiliation(s)
- M Korobko
- Institut für Quantenphysik und Zentrum für Optische Quantentechnologien der Universität Hamburg, 5 Luruper Chaussee 149, 22761 Hamburg, Germany
| | - J Südbeck
- Institut für Quantenphysik und Zentrum für Optische Quantentechnologien der Universität Hamburg, 5 Luruper Chaussee 149, 22761 Hamburg, Germany
| | - S Steinlechner
- Faculty of Science and Engineering, Maastricht University, Duboisdomein 30, 6229 GT Maastricht, Netherlands
- Nikhef, Science Park 105, 1098 XG Amsterdam, Netherlands
| | - R Schnabel
- Institut für Quantenphysik und Zentrum für Optische Quantentechnologien der Universität Hamburg, 5 Luruper Chaussee 149, 22761 Hamburg, Germany
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91
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Duerr PM, Wolf WJ. Methodological reflections on the MOND/dark matter debate. STUDIES IN HISTORY AND PHILOSOPHY OF SCIENCE 2023; 101:1-23. [PMID: 37531699 DOI: 10.1016/j.shpsa.2023.07.001] [Citation(s) in RCA: 1] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/10/2022] [Revised: 06/28/2023] [Accepted: 07/07/2023] [Indexed: 08/04/2023]
Abstract
The paper re-examines the principal methodological questions, arising in the debate over the cosmological standard model's postulate of Dark Matter vs. rivalling proposals that modify standard (Newtonian and general-relativistic) gravitational theory, the so-called Modified Newtonian Dynamics (MOND) and its subsequent extensions. What to make of such seemingly radical challenges of cosmological orthodoxy? In the first part of our paper, we assess MONDian theories through the lens of key ideas of major 20th century philosophers of science (Popper, Kuhn, Lakatos, and Laudan), thereby rectifying widespread misconceptions and misapplications of these ideas common in the pertinent MOND-related literature. None of these classical methodological frameworks, which render precise and systematise the more intuitive judgements prevalent in the scientific community, yields a favourable verdict on MOND and its successors-contrary to claims in the MOND-related literature by some of these theories' advocates; the respective theory appraisals are largely damning. Drawing on these insights, the paper's second part zooms in on the most common complaint about MONDian theories, their ad-hocness. We demonstrate how the recent coherentist model of ad-hocness captures, and fleshes out, the underlying-but too often insufficiently articulated-hunches underlying this critique. MONDian theories indeed come out as severely ad hoc: they do not cohere well with either theoretical or empirical-factual background knowledge. In fact, as our complementary comparison with the cosmological standard model's Dark Matter postulate shows, with respect to ad-hocness, MONDian theories fare worse than the cosmological standard model.
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Affiliation(s)
- Patrick M Duerr
- Martin Buber Society of Fellows for Research in the Humanities and Social Sciences, Hebrew University of Jerusalem, Israel; Faculty of Philosophy, University of Oxford, UK.
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92
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Dias ÓJC, Gibbons GW, Santos JE, Way B. Static Black Binaries in de Sitter Space. PHYSICAL REVIEW LETTERS 2023; 131:131401. [PMID: 37832001 DOI: 10.1103/physrevlett.131.131401] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/07/2023] [Accepted: 07/31/2023] [Indexed: 10/15/2023]
Abstract
We construct the first four-dimensional multiple black hole solution of general relativity with a positive cosmological constant. The solution consists of two static black holes whose gravitational attraction is balanced by the cosmic expansion. These static binaries provide the first four-dimensional example of nonuniqueness in general relativity without matter.
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Affiliation(s)
- Óscar J C Dias
- STAG Research Centre and Mathematical Sciences, University of Southampton, Highfield Campus, SO17 1BJ, United Kingdom
| | - Gary W Gibbons
- DAMTP, Centre for Mathematical Sciences, University of Cambridge, Wilberforce Road, Cambridge CB3 0WA, United Kingdom
| | - Jorge E Santos
- DAMTP, Centre for Mathematical Sciences, University of Cambridge, Wilberforce Road, Cambridge CB3 0WA, United Kingdom
| | - Benson Way
- Departament de Física Quàntica i Astrofísica, Institut de Ciències del Cosmos Universitat de Barcelona, Martí i Franquès, 1, E-08028 Barcelona, Spain
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93
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Hughes WJ, Doherty TH, Blackmore JA, Horak P, Goodwin JF. Mode mixing and losses in misaligned microcavities. OPTICS EXPRESS 2023; 31:32619-32636. [PMID: 37859061 DOI: 10.1364/oe.496981] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/21/2023] [Accepted: 08/11/2023] [Indexed: 10/21/2023]
Abstract
We present a study on the optical losses of Fabry-Pérot cavities subject to realistic transverse mirror misalignment. We consider mirrors of the two most prevalent surface forms: idealised spherical depressions, and Gaussian profiles generated by laser ablation. We first describe the mode mixing phenomena seen in the spherical mirror case and compare to the frequently-used clipping model, observing close agreement in the predicted diffraction loss, but with the addition of protective mode mixing at transverse degeneracies. We then discuss the Gaussian mirror case, detailing how the varying surface curvature across the mirror leads to complex variations in round trip loss and mode profile. In light of the severe mode distortion and strongly elevated loss predicted for many cavity lengths and transverse alignments when using Gaussian mirrors, we suggest that the consequences of mirror surface profile are carefully considered when designing cavity experiments.
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94
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Blanchet L, Faye G, Henry Q, Larrouturou F, Trestini D. Gravitational-Wave Phasing of Quasicircular Compact Binary Systems to the Fourth-and-a-Half Post-Newtonian Order. PHYSICAL REVIEW LETTERS 2023; 131:121402. [PMID: 37802935 DOI: 10.1103/physrevlett.131.121402] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/16/2023] [Accepted: 07/10/2023] [Indexed: 10/08/2023]
Abstract
The inspiral phase of gravitational waves emitted by spinless compact binary systems is derived through the fourth-and-a-half post-Newtonian (4.5PN) order beyond quadrupole radiation, and the leading amplitude mode (ℓ,m)=(2,2) is obtained at 4PN order. We also provide the radiated flux, as well as the phase in the stationary phase approximation. Rough numerical estimates for the contribution of each PN order are provided for typical systems observed by current and future gravitational wave detectors.
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Affiliation(s)
- Luc Blanchet
- 𝒢ℝϵℂ𝒪, Institut d'Astrophysique de Paris, UMR 7095, CNRS, Sorbonne Université, 98bis boulevard Arago, 75014 Paris, France
| | - Guillaume Faye
- 𝒢ℝϵℂ𝒪, Institut d'Astrophysique de Paris, UMR 7095, CNRS, Sorbonne Université, 98bis boulevard Arago, 75014 Paris, France
- Centre for Strings, Gravitation and Cosmology, Department of Physics, Indian Institute of Technology Madras, Chennai 600036, India
| | - Quentin Henry
- Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-14476 Potsdam, Germany
| | | | - David Trestini
- 𝒢ℝϵℂ𝒪, Institut d'Astrophysique de Paris, UMR 7095, CNRS, Sorbonne Université, 98bis boulevard Arago, 75014 Paris, France
- Laboratoire Univers et Théories, Observatoire de Paris, Université PSL, Université Paris Cité, CNRS, F-92190 Meudon, France
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95
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Herdeiro CAR, Radu E. Two Spinning Black Holes Balanced by Their Synchronized Scalar Hair. PHYSICAL REVIEW LETTERS 2023; 131:121401. [PMID: 37802955 DOI: 10.1103/physrevlett.131.121401] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/30/2023] [Accepted: 08/08/2023] [Indexed: 10/08/2023]
Abstract
General relativity minimally coupled to a massive, free, complex scalar field, is shown to allow asymptotically flat solutions, nonsingular on and outside the event horizon, describing two spinning black holes (2sBHs) in equilibrium, with coaxial, aligned angular momenta. The 2sBHs configurations bifurcate from solutions describing dipolar spinning boson stars. The BHs emerge at equilibrium points diagnosed by a test particle analysis and illustrated by a Newtonian analog. The individual BH "charges" are mass and angular momentum only. Equilibrium is due to the scalar environment, acting as a (compact) dipolar field, providing a lift against their mutual attraction, making the 2sBHs (h)airborne. We explore the 2sBHs domain of solutions and its main features.
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Affiliation(s)
- Carlos A R Herdeiro
- Departamento de Matemática da Universidade de Aveiro and CIDMA, Campus de Santiago, 3810-183 Aveiro, Portugal
| | - Eugen Radu
- Departamento de Matemática da Universidade de Aveiro and CIDMA, Campus de Santiago, 3810-183 Aveiro, Portugal
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96
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Cayuso R, Figueras P, França T, Lehner L. Self-Consistent Modeling of Gravitational Theories beyond General Relativity. PHYSICAL REVIEW LETTERS 2023; 131:111403. [PMID: 37774295 DOI: 10.1103/physrevlett.131.111403] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 03/23/2023] [Accepted: 08/08/2023] [Indexed: 10/01/2023]
Abstract
The majority of extensions to general relativity (GR) display mathematical pathologies-higher derivatives, character change in equations that can be classified within partial differential equation theory, and even unclassifiable ones-that cause severe difficulties to study them, especially in dynamical regimes. We present here an approach that enables their consistent treatment and extraction of physical consequences. We illustrate this method in the context of single and merging black holes in a highly challenging beyond GR theory.
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Affiliation(s)
- Ramiro Cayuso
- Perimeter Institute for Theoretical Physics, 31 Caroline Street North, Waterloo, Ontario N2L 2Y5, Canada
- Department of Physics and Astronomy, University of Waterloo, Waterloo, Ontario N2L 3G1, Canada
| | - Pau Figueras
- School of Mathematical Sciences, Queen Mary University of London, Mile End Road, London E1 4NS, United Kingdom
| | - Tiago França
- School of Mathematical Sciences, Queen Mary University of London, Mile End Road, London E1 4NS, United Kingdom
| | - Luis Lehner
- Perimeter Institute for Theoretical Physics, 31 Caroline Street North, Waterloo, Ontario N2L 2Y5, Canada
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97
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Cardoso V, Vicente R, Zhong Z. Energy Extraction from Q-balls and Other Fundamental Solitons. PHYSICAL REVIEW LETTERS 2023; 131:111602. [PMID: 37774264 DOI: 10.1103/physrevlett.131.111602] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 03/07/2023] [Revised: 05/28/2023] [Accepted: 07/25/2023] [Indexed: 10/01/2023]
Abstract
Energy exchange mechanisms have important applications in particle physics, gravity, fluid mechanics, and practically every field in physics. In this Letter we show, both in the frequency and time domain, that energy enhancement is possible for waves scattering off fundamental solitons (time-periodic localized structures of bosonic fields), without the need for rotation nor translational motion. We use two-dimensional Q-balls as a test bed, providing the correct criteria for energy amplification, as well as the respective amplification factors, and we discuss possible instability mechanisms. Our results lend support to the qualitative picture drawn in Saffin et al. [preceding Letter, Q-ball superradiance, Phys. Rev. Lett. 131, 111601 (2023).PRLTAO0031-900710.1103/PhysRevLett.131.111601]; however, we show that this enhancement mechanism is not of superradiant type, but instead is a "blueshiftlike" energy exchange between scattering states induced by the background Q-ball, which should occur generically for any time-periodic fundamental soliton. This mechanism does not seem to lead to instabilities.
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Affiliation(s)
- Vitor Cardoso
- Niels Bohr International Academy, Niels Bohr Institute, Blegdamsvej 17, 2100 Copenhagen, Denmark
- CENTRA, Departamento de Física, Instituto Superior Técnico-IST, Universidade de Lisboa-UL, Avenida Rovisco Pais 1, 1049-001 Lisboa, Portugal
| | - Rodrigo Vicente
- Institut de Fisica d'Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, 08193 Bellaterra (Barcelona), Spain
| | - Zhen Zhong
- CENTRA, Departamento de Física, Instituto Superior Técnico-IST, Universidade de Lisboa-UL, Avenida Rovisco Pais 1, 1049-001 Lisboa, Portugal
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98
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Foglieni M, Pantiri M, Di Dio E, Castorina E. Large Scale Limit of the Observed Galaxy Power Spectrum. PHYSICAL REVIEW LETTERS 2023; 131:111201. [PMID: 37774263 DOI: 10.1103/physrevlett.131.111201] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 03/13/2023] [Accepted: 08/15/2023] [Indexed: 10/01/2023]
Abstract
The large scale limit of the galaxy power spectrum provides a unique window into the early Universe through a possible detection of scale dependent bias produced by primordial non Gaussianities. On such large scales, relativistic effects could become important and be confused for a primordial signal. In this Letter we provide the first consistent estimate of such effects in the observed galaxy power spectrum, and discuss their possible degeneracy with local primordial non Gaussianities. We also clarify the physical differences between the two signatures, as revealed by their different sensitivity to the large scale gravitational potential. Our results indicate that, while relativistic effects could easily account for 10% of the observed power spectrum, the subset of those with a similar scale dependence to a primordial signal can be safely ignored for current galaxy surveys, but it will become relevant for future observational programs.
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Affiliation(s)
- Matteo Foglieni
- Leibniz Supercomputing Centre (LRZ), Boltzmannstraße 1, 85748 Garching bei München, Germany
- Dipartimento di Fisica "Aldo Pontremoli", Universita' degli Studi di Milano, Via Celoria 16, 20133 Milan, Italy
| | - Mattia Pantiri
- Dipartimento di Fisica "Aldo Pontremoli", Universita' degli Studi di Milano, Via Celoria 16, 20133 Milan, Italy
| | - Enea Di Dio
- Theoretical Physics Department, CERN, 1211 Geneva 23, Switzerland
| | - Emanuele Castorina
- Dipartimento di Fisica "Aldo Pontremoli", Universita' degli Studi di Milano, Via Celoria 16, 20133 Milan, Italy
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99
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Meena HK, Pant B, Singh BK. Controllable experimental modulation of high-order Laguerre-Gaussian laser modes. JOURNAL OF THE OPTICAL SOCIETY OF AMERICA. A, OPTICS, IMAGE SCIENCE, AND VISION 2023; 40:1770-1778. [PMID: 37707014 DOI: 10.1364/josaa.499212] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/29/2023] [Accepted: 08/09/2023] [Indexed: 09/15/2023]
Abstract
High-order helical and sinusoidal Laguerre-Gaussian (LG) laser modes have uneven energy distribution among their multiple concentric vortex core rings and lobes, respectively. Here, we explore an experimental method to reshuffle the optical energy among their multiple concentric vortex core rings and lobes of high-order LG modes in a controllable manner. We numerically designed a diffractive optical element displayed over a spatial light modulator to rearrange optical energy among multiple concentric vortex core rings. This changes outer low-intensity concentric vortex core rings into high-intensity vortex core rings of high-order helical LG modes at the Fourier plane. The precise generation of a high-order modulated helical LG laser mode has a maximum number of highly intense concentric vortex core rings compared to known standard helical LG modes. Further, this method is extended to high-order sinusoidal LG modes consisting of both low- and high-intensity lobes to realize modulated sinusoidal LG modes with a maximum number of highly intense lobes in a controllable manner. We envisage that the modulated helical and sinusoidal high-order LG modes may surpass standard LG modes in many applications where highly intense rings and lobes are crucial, as in particle manipulation of micro- and nanoparticles, and optical lithography.
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100
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Käding C, Pitschmann M, Voith C. Dilaton-induced open quantum dynamics. THE EUROPEAN PHYSICAL JOURNAL. C, PARTICLES AND FIELDS 2023; 83:767. [PMID: 37662873 PMCID: PMC10471684 DOI: 10.1140/epjc/s10052-023-11939-4] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/06/2023] [Accepted: 08/08/2023] [Indexed: 09/05/2023]
Abstract
In modern cosmology, scalar fields with screening mechanisms are often used as explanations for phenomena like dark energy or dark matter. Amongst a zoo of models, the environment dependent dilaton, screened by the Polyakov-Damour mechanism, is one of the least constrained ones. Using recently developed path integral tools for directly computing reduced density matrices, we study the open quantum dynamics of a probe, modelled by another real scalar field, induced by interactions with an environment comprising fluctuations of a dilaton. As the leading effect, we extract a correction to the probe's unitary evolution, which can be observed as a frequency shift. Assuming the scalar probe to roughly approximate a cold atom in matter wave interferometry, we show that comparing the predicted frequency shifts in two experimentally distinct setups has the potential to exclude large parts of the dilaton parameter space.
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Affiliation(s)
- Christian Käding
- Technische Universität Wien, Atominstitut, Stadionallee 2, 1020 Vienna, Austria
| | - Mario Pitschmann
- Technische Universität Wien, Atominstitut, Stadionallee 2, 1020 Vienna, Austria
| | - Caroline Voith
- Technische Universität Wien, Atominstitut, Stadionallee 2, 1020 Vienna, Austria
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