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Dergachev VD, Tran Tan HB, Varganov SA, Derevianko A. Effect of Extreme Variations of Fundamental Constants on the Structure of Atoms and Molecules. J Phys Chem Lett 2024; 15:4111-4116. [PMID: 38589052 DOI: 10.1021/acs.jpclett.4c00599] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 04/10/2024]
Abstract
The fundamental constants (FCs) of physics are promoted to dynamic quantities in modern theories. So far most of the literature focused on small fractional variations in the values of FCs. In this paper, we investigate the novel regime of extreme but transient variations of FCs. We focus on the speed of light (c) and show that its variation can dramatically change the electronic structure and chemistry of atoms and molecules. These changes are induced by increased relativistic effects when c is reduced from its nominal value. To model these changes, we solve the fully relativistic Dirac equation at different values of c. We show that at extreme variations of c, the periodic table is truncated, the nominal ground states of atoms can change, water fails to serve as a universal solvent, and the ammonia molecule becomes planar.
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Affiliation(s)
- Vsevolod D Dergachev
- Department of Chemistry, University of Nevada, Reno, 1664 North Virginia Street, Reno, Nevada 89557-0216, United States
| | - Hoang Bao Tran Tan
- Department of Physics, University of Nevada, Reno, 1664 North Virginia Street, Reno, Nevada 89557-0216, United States
- Los Alamos National Laboratory, P.O. Box 1663, Los Alamos, New Mexico 87545, United States
| | - Sergey A Varganov
- Department of Chemistry, University of Nevada, Reno, 1664 North Virginia Street, Reno, Nevada 89557-0216, United States
| | - Andrei Derevianko
- Department of Physics, University of Nevada, Reno, 1664 North Virginia Street, Reno, Nevada 89557-0216, United States
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2
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Davis ED. Oklo natural fission reactors and dynamical models of dark energy. Radiat Prot 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] [What about the content of this article? (0)] [Affiliation(s)] [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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3
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Trachenko K. Viscosity and diffusion in life processes and tuning of fundamental constants. Rep Prog Phys 2023; 86:112601. [PMID: 37811635 DOI: 10.1088/1361-6633/acfd3e] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [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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4
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Shamir L. Asymmetry in Galaxy Spin Directions—Analysis of Data from DES and Comparison to Four Other Sky Surveys. Universe 2022; 8:397. [DOI: 10.3390/universe8080397] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 02/01/2023]
Abstract
The paper shows an analysis of the large-scale distribution of galaxy spin directions of 739,286 galaxies imaged by DES. The distribution of the spin directions of the galaxies exhibits a large-scale dipole axis. Comparison of the location of the dipole axis to a similar analysis with data from SDSS, Pan-STARRS, and DESI Legacy Survey shows that all sky surveys exhibit dipole axes within 52° or less from each other, well within 1σ error, while non-random distribution is unexpected, the findings are consistent across all sky surveys, regardless of the telescope or whether the data were annotated manually or automatically. Possible errors that can lead to the observation are discussed. The paper also discusses previous studies showing opposite conclusions and analyzes the decisions that led to these results. Although the observation is provocative, and further research will be required, the existing evidence justifies considering the contention that galaxy spin directions as observed from Earth are not necessarily randomly distributed. Possible explanations can be related to mature cosmological theories, but also to the internal structure of galaxies.
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Chae E, Nakashima K, Yoshioka K. Dual optical frequency combs with ultra-low relative phase jitters from 550 nm to 1020 nm for precision spectroscopy. Opt Express 2022; 30:18703-18712. [PMID: 36221666 DOI: 10.1364/oe.458735] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 03/18/2022] [Accepted: 05/04/2022] [Indexed: 06/16/2023]
Abstract
Here, ultra-low relative phase jitters over a wide optical spectrum were achieved for dual Ti:Sapphire optical frequency combs. The two optical frequency combs were independently phase-locked to a Sr optical lattice clock laser delivered through a commercial optical fiber network. We confirmed that the relative phase jitters between the two combs integrated from 8.3 mHz to 200 kHz were below 1 rad, corresponding to a relative linewidth of below 8.3 mHz, over the entire wavelength of the optical frequency combs ranging from 550 nm to 1020 nm. Our work paves the way for ultrahigh-precision dual-comb spectroscopy covering a wide optical spectral range with a simple setup, and provides an absolute optical frequency reference with great stability over a wide range of wavelengths.
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Brunet TDP. Local causation. Synthese 2021; 199:10885-10908. [PMID: 34970012 PMCID: PMC8668861 DOI: 10.1007/s11229-021-03272-8] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 10/21/2020] [Accepted: 06/17/2021] [Indexed: 06/14/2023]
Abstract
The counterfactual and regularity theories are universal accounts of causation. I argue that these should be generalized to produce local accounts of causation. A hallmark of universal accounts of causation is the assumption that apparent variation in causation between locations must be explained by differences in background causal conditions, by features of the causal-nexus or causing-complex. The local account of causation presented here rejects this assumption, allowing for genuine variation in causation to be explained by differences in location. I argue that local accounts of causation are plausible, and have pragmatic, empirical and theoretical advantages over universal accounts. I then report on the use of presheaves as models of local causation. The use of presheaves as models of local variation has precedents in algebraic geometry, category theory and physics; they are here used as models of local causal variation. The paper presents this idea as stemming from an approach using presheaves as models of local truth. Finally, I argue that a proper balance between universal and local causation can be assuaged by moving from presheaves to fully-fledged sheaf models.
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Affiliation(s)
- T. D. P. Brunet
- Department of History and Philosophy of Science, University of Cambridge, Free School Lane, Cambridge, CB2 3RH UK
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Singal A. Our Peculiar Motion Inferred from Number Counts of Mid Infra Red AGNs and the Discordance Seen with the Cosmological Principle. Universe 2021; 7:107. [DOI: 10.3390/universe7040107] [Citation(s) in RCA: 7] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
Abstract
According to the Cosmological Principle, the Universe is isotropic and no preferred direction would be seen by an observer that might be stationary with respect to the expanding cosmic fluid. However, because of observer’s partaking in the solar system peculiar motion, there would appear in some of the observed properties of the Cosmos a dipole anisotropy, which could in turn be exploited to determine the peculiar motion of the solar system. The dipole anisotropy in the Cosmic Microwave Background Radiation (CMBR) has given a peculiar velocity vector 370 km s−1 along l=264∘,b=48∘. However, some other dipoles, for instance, from the number counts, sky brightness or redshift distributions in large samples of distant Active Galactic Nuclei (AGNs), have yielded values of the peculiar velocity many times larger than that from the CMBR, though surprisingly, in all cases the directions agreed with the CMBR dipole. Here we determine our peculiar motion from a sample of 0.28 million AGNs, selected from the Mid Infra Red Active Galactic Nuclei (MIRAGN) sample comprising more than a million sources. From this, we find a peculiar velocity, which is more than four times the CMBR value, although the direction seems to be within ∼2σ of the CMBR dipole. A genuine value of the solar peculiar velocity should be the same irrespective of the data or the technique employed to estimate it. Therefore, such discordant dipole amplitudes might mean that the explanation for these dipoles, including that of the CMBR, might in fact be something else. The observed fact that the direction in all cases is the same, though obtained from completely independent surveys using different instruments and techniques, by different sets of people employing different computing routines, might nonetheless indicate that these dipoles are not merely due to some systematics, otherwise why would they all be pointing along the same direction. It might instead suggest a preferred direction in the Universe, implying a genuine anisotropy, which would violate the Cosmological Principle, the core of the modern cosmology.
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Zhang Y, Lin QN, Yang T, Yin JP, Wang HL. Theoretical calculation on isotope shifts of N(I). CHINESE J CHEM PHYS 2020. [DOI: 10.1063/1674-0068/cjcp2003035] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/15/2022]
Affiliation(s)
- Yan Zhang
- State Key Laboratory of Precision Spectroscopy, East China Normal University, Shanghai 200241, China
| | - Qing-ning Lin
- State Key Laboratory of Precision Spectroscopy, East China Normal University, Shanghai 200241, China
| | - Tao Yang
- State Key Laboratory of Precision Spectroscopy, East China Normal University, Shanghai 200241, China
| | - Jian-ping Yin
- State Key Laboratory of Precision Spectroscopy, East China Normal University, Shanghai 200241, China
| | - Hai-ling Wang
- State Key Laboratory of Precision Spectroscopy, East China Normal University, Shanghai 200241, China
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Le T. Stringent limit on space-time variation of fine-structure constant using high-resolution of quasar spectra. Heliyon 2020; 6:e05011. [PMID: 32995647 PMCID: PMC7511822 DOI: 10.1016/j.heliyon.2020.e05011] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 03/31/2020] [Revised: 06/19/2020] [Accepted: 09/17/2020] [Indexed: 11/13/2022] Open
Abstract
We have obtained a new limit on the space-time variation of the fine-structure constant(α=e24πε0ℏc)using the observations of Mg II line in quasar J110325-264515 spectra with redshiftzabs=1.8389. The obtained parameter isΔα/α=(−0.155±0.728)×10−6. It was derived from the comparison between the quasar J110325-264515 spectra and the laboratory sample spectra. The obtained result appears as a new highly sensitive probe of the cosmological variability of the fine-structure constant. From the relative spectra of the Mg II, we found the most stringent constraint up today onΔα/αcomparing to the previously published results.
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Wilczynska MR, Webb JK, Bainbridge M, Barrow JD, Bosman SEI, Carswell RF, Dąbrowski MP, Dumont V, Lee CC, Leite AC, Leszczyńska K, Liske J, Marosek K, Martins CJAP, Milaković D, Molaro P, Pasquini L. Four direct measurements of the fine-structure constant 13 billion years ago. Sci Adv 2020; 6:6/17/eaay9672. [PMID: 32917582 PMCID: PMC7182409 DOI: 10.1126/sciadv.aay9672] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 08/01/2019] [Accepted: 01/15/2020] [Indexed: 06/11/2023]
Abstract
Observations of the redshift z = 7.085 quasar J1120+0641 are used to search for variations of the fine structure constant, α, over the redshift range 5.5 to 7.1. Observations at z = 7.1 probe the physics of the universe at only 0.8 billion years old. These are the most distant direct measurements of α to date and the first measurements using a near-IR spectrograph. A new AI analysis method is employed. Four measurements from the x-shooter spectrograph on the Very Large Telescope (VLT) constrain changes in a relative to the terrestrial value (α0). The weighted mean electromagnetic force in this location in the universe deviates from the terrestrial value by Δα/α = (α z - α0)/α0 = (-2.18 ± 7.27) × 10-5, consistent with no temporal change. Combining these measurements with existing data, we find a spatial variation is preferred over a no-variation model at the 3.9σ level.
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Affiliation(s)
| | - John K Webb
- University of New South Wales Sydney, Sydney, NSW 2052, Australia.
| | - Matthew Bainbridge
- College of Science and Engineering, University of Leicester, University Road, Leicester LE17RH, UK
| | - John D Barrow
- DAMTP, Centre for Mathematical Sciences, University of Cambridge, Cambridge CB3 0WA, UK
| | - Sarah E I Bosman
- Department of Physics and Astronomy, University College London, London WC1E 6BT, UK
| | | | - Mariusz P Dąbrowski
- Institute of Physics, University of Szczecin, Wielkopolska 15, 70-451 Szczecin, Poland
| | - Vincent Dumont
- Computational Research Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA
| | - Chung-Chi Lee
- DAMTP, Centre for Mathematical Sciences, University of Cambridge, Cambridge CB3 0WA, UK
| | - Ana Catarina Leite
- Centro de Astrofísica da Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal
- Instituto de Astrofísica e Ciências do Espaço, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal
- Faculdade de Ciências, Universidade do Porto, Rua do Campo Alegre, 4150-007 Porto, Portugal
| | - Katarzyna Leszczyńska
- Institute of Physics, University of Szczecin, Wielkopolska 15, 70-451 Szczecin, Poland
| | - Jochen Liske
- Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, D-21029 Hamburg, Germany
| | - Konrad Marosek
- Maritime University, Wały Chrobrego 1-2, 70-500 Szczecin, Poland
| | - Carlos 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, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal
| | - Dinko Milaković
- European Southern Observatory, 85748 Garching bei München, Germany
- Ludwig-Maximilians-Universität, 80799 Munich, Germany
| | - Paolo Molaro
- National Institute for Astrophysics, Astronomical Observatory of Trieste, Via G.B. Tiepolo 11, I34134, Italy
| | - Luca Pasquini
- European Southern Observatory, 85748 Garching bei München, Germany
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Le TD. New Limit on Space-Time Variations in the Proton-to-Electron Mass Ratio from Analysis of Quasar J110325-264515 Spectra. Symmetry (Basel) 2020; 12:344. [DOI: 10.3390/sym12030344] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 12/25/2022] Open
Abstract
Astrophysical tests of current values for dimensionless constants known on Earth, such as the fine-structure constant, α , and proton-to-electron mass ratio, μ = m p / m e , are communicated using data from high-resolution quasar spectra in different regions or epochs of the universe. The symmetry wavelengths of [Fe II] lines from redshifted quasar spectra of J110325-264515 and their corresponding values in the laboratory were combined to find a new limit on space-time variations in the proton-to-electron mass ratio, ∆ μ / μ = ( 0.096 ± 0.182 ) × 10 − 7 . The results show how the indicated astrophysical observations can further improve the accuracy and space-time variations of physics constants.
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Abstract
In the first part we present the number theoretical properties of the Riemann zeta function and formulate the Riemann hypothesis. In the second part we review some physical problems related to this hypothesis: the Polya-Hilbert conjecture, the links with random matrix theory, relation with the Lee-Yang theorem on the zeros of the partition function and phase transitions, random walks, billiards etc.
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Affiliation(s)
- Marek Wolf
- Faculty of Mathematics and Natural Sciences, Cardinal Stefan Wyszynski University, ul. Woycickiego 1/3, PL-01-938 Warsaw, Poland
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14
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Hees A, Do T, Roberts BM, Ghez AM, Nishiyama S, Bentley RO, Gautam AK, Jia S, Kara T, Lu JR, Saida H, Sakai S, Takahashi M, Takamori Y. Search for a Variation of the Fine Structure Constant around the Supermassive Black Hole in Our Galactic Center. Phys Rev Lett 2020; 124:081101. [PMID: 32167338 DOI: 10.1103/physrevlett.124.081101] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/21/2019] [Accepted: 01/23/2020] [Indexed: 06/10/2023]
Abstract
Searching for space-time variations of the constants of Nature is a promising way to search for new physics beyond general relativity and the standard model motivated by unification theories and models of dark matter and dark energy. We propose a new way to search for a variation of the fine-structure constant using measurements of late-type evolved giant stars from the S star cluster orbiting the supermassive black hole in our Galactic Center. A measurement of the difference between distinct absorption lines (with different sensitivity to the fine structure constant) from a star leads to a direct estimate of a variation of the fine structure constant between the star's location and Earth. Using spectroscopic measurements of five stars, we obtain a constraint on the relative variation of the fine structure constant below 10^{-5}. This is the first time a varying constant of nature is searched for around a black hole and in a high gravitational potential. This analysis shows new ways the monitoring of stars in the Galactic Center can be used to probe fundamental physics.
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Affiliation(s)
- A Hees
- SYRTE, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, LNE, 61 avenue de l'Observatoire 75014 Paris, France
| | - T Do
- Department of Physics and Astronomy, University of California, Los Angeles, California 90095, USA
| | - B M Roberts
- SYRTE, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, LNE, 61 avenue de l'Observatoire 75014 Paris, France
- School of Mathematics and Physics, The University of Queensland, Brisbane, Queensland 4072, Australia
| | - A M Ghez
- Department of Physics and Astronomy, University of California, Los Angeles, California 90095, USA
| | - S Nishiyama
- Miyagi University of Education, 149 Aramaki-aza-aoba, Aoba-ku, Sendai, Miyagi 980-0845, Japan
| | - R O Bentley
- Department of Physics and Astronomy, University of California, Los Angeles, California 90095, USA
| | - A K Gautam
- Department of Physics and Astronomy, University of California, Los Angeles, California 90095, USA
| | - S Jia
- Astronomy Department, University of California, Berkeley, California 94720, USA
| | - T Kara
- Miyagi University of Education, 149 Aramaki-aza-aoba, Aoba-ku, Sendai, Miyagi 980-0845, Japan
| | - J R Lu
- Astronomy Department, University of California, Berkeley, California 94720, USA
| | - H Saida
- Daido University, 10-3 Takiharu-cho, Minami-ku, Nagoya, Aichi 457-8530, Japan
| | - S Sakai
- Department of Physics and Astronomy, University of California, Los Angeles, California 90095, USA
| | - M Takahashi
- Aichi University of Education, 1 Hirosawa, Igaya-cho, Kariya, Aichi 448-8542, Japan
| | - Y Takamori
- National Institute of Technology, Wakayama College, 77 Noshima, Nada-cho, Gobo, Wakayama 644-0023, Japan
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Abstract
I used observed spectra from the white-dwarf star G191-B2B to constrain the spatial and temporal variation of the fine-structure constant,[...]
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Chae E, Nakashima K, Ikeda T, Sugiyama K, Yoshioka K. Direct phase-locking of a Ti:Sapphire optical frequency comb to a remote optical frequency standard. Opt Express 2019; 27:15649-15661. [PMID: 31163759 DOI: 10.1364/oe.27.015649] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/02/2019] [Accepted: 05/06/2019] [Indexed: 06/09/2023]
Abstract
We report on an ultralow noise optical frequency transfer from a remotely located Sr optical lattice clock laser to a Ti:Sapphire optical frequency comb through telecom-wavelength optical fiber networks. The inherent narrow linewidth of the Ti:Sapphire optical frequency comb eliminates the need for a local reference high-finesse cavity. The relative fractional frequency instability of the optical frequency comb with respect to the remote optical reference was 6.7(1) × 10-18 at 1 s and 1.05(3) × 10-19 at 1,000 s including a 2.9 km-long fiber network. This ensured the optical frequency comb had the same precision as the optical standard. Our result paves the way for ultrahigh-precision spectroscopy and conversion of the highly precise optical frequency to radio frequencies in a simpler setup.
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18
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Le TD. An Updated Constraint on Variations of the Fine-Structure Constant Using Wavelengths of Fe II Absorption Line Multiplets. Symmetry (Basel) 2018; 10:722. [DOI: 10.3390/sym10120722] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/16/2022] Open
Abstract
A new stringent limit relating to the variation of the fine-structure constant (α= e2/4πε0ℏc) has been extracted from Ritz wavelengths of 27 quasi_stellar object (QSO) absorption spectra lines of Fe II. The calculation was combined with laboratory wavelengths and QSO spectra to obtain the result ∆α/α=(0.027±0.832)×10-6. This result suggests how dedicated astrophysical estimations can improve these limits in the future and can also constrain space_time variations.
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Wcisło P, Ablewski P, Beloy K, Bilicki S, Bober M, Brown R, Fasano R, Ciuryło R, Hachisu H, Ido T, Lodewyck J, Ludlow A, McGrew W, Morzyński P, Nicolodi D, Schioppo M, Sekido M, Le Targat R, Wolf P, Zhang X, Zjawin B, Zawada M. New bounds on dark matter coupling from a global network of optical atomic clocks. Sci Adv 2018; 4:eaau4869. [PMID: 30539146 PMCID: PMC6286165 DOI: 10.1126/sciadv.aau4869] [Citation(s) in RCA: 29] [Impact Index Per Article: 4.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 06/14/2018] [Accepted: 11/07/2018] [Indexed: 06/09/2023]
Abstract
We report on the first Earth-scale quantum sensor network based on optical atomic clocks aimed at dark matter (DM) detection. Exploiting differences in the susceptibilities to the fine-structure constant of essential parts of an optical atomic clock, i.e., the cold atoms and the optical reference cavity, we can perform sensitive searches for DM signatures without the need for real-time comparisons of the clocks. We report a two orders of magnitude improvement in constraints on transient variations of the fine-structure constant, which considerably improves the detection limit for the standard model (SM)-DM coupling. We use Yb and Sr optical atomic clocks at four laboratories on three continents to search for both topological defect and massive scalar field candidates. No signal consistent with a DM coupling is identified, leading to considerably improved constraints on the DM-SM couplings.
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Affiliation(s)
- P. Wcisło
- Institute of Physics, Faculty of Physics, Astronomy and Informatics, Nicolaus Copernicus University, Grudziądzka 5, PL-87-100 Toruń, Poland
- JILA, National Institute of Standards and Technology and the University of Colorado, Department of Physics, University of Colorado, Boulder, CO 80309–0440, USA
| | - P. Ablewski
- Institute of Physics, Faculty of Physics, Astronomy and Informatics, Nicolaus Copernicus University, Grudziądzka 5, PL-87-100 Toruń, Poland
| | - K. Beloy
- National Institute of Standards and Technology, 325 Broadway, Boulder, CO 80305–3337, USA
| | - S. Bilicki
- Institute of Physics, Faculty of Physics, Astronomy and Informatics, Nicolaus Copernicus University, Grudziądzka 5, PL-87-100 Toruń, Poland
- LNE-SYRTE, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, 61 avenue de l’Observatoire 75014 Paris, France
| | - M. Bober
- Institute of Physics, Faculty of Physics, Astronomy and Informatics, Nicolaus Copernicus University, Grudziądzka 5, PL-87-100 Toruń, Poland
| | - R. Brown
- National Institute of Standards and Technology, 325 Broadway, Boulder, CO 80305–3337, USA
| | - R. Fasano
- National Institute of Standards and Technology, 325 Broadway, Boulder, CO 80305–3337, USA
- Department of Physics, University of Colorado, Boulder, CO 80309–0440, USA
| | - R. Ciuryło
- Institute of Physics, Faculty of Physics, Astronomy and Informatics, Nicolaus Copernicus University, Grudziądzka 5, PL-87-100 Toruń, Poland
| | - H. Hachisu
- National Institute of Information and Communications Technology, 4-2-1 Nukuikitamachi, Koganei, 184-8795 Tokyo, Japan
| | - T. Ido
- National Institute of Information and Communications Technology, 4-2-1 Nukuikitamachi, Koganei, 184-8795 Tokyo, Japan
| | - J. Lodewyck
- LNE-SYRTE, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, 61 avenue de l’Observatoire 75014 Paris, France
| | - A. Ludlow
- National Institute of Standards and Technology, 325 Broadway, Boulder, CO 80305–3337, USA
- Department of Physics, University of Colorado, Boulder, CO 80309–0440, USA
| | - W. McGrew
- National Institute of Standards and Technology, 325 Broadway, Boulder, CO 80305–3337, USA
- Department of Physics, University of Colorado, Boulder, CO 80309–0440, USA
| | - P. Morzyński
- Institute of Physics, Faculty of Physics, Astronomy and Informatics, Nicolaus Copernicus University, Grudziądzka 5, PL-87-100 Toruń, Poland
- National Institute of Information and Communications Technology, 4-2-1 Nukuikitamachi, Koganei, 184-8795 Tokyo, Japan
| | - D. Nicolodi
- National Institute of Standards and Technology, 325 Broadway, Boulder, CO 80305–3337, USA
| | - M. Schioppo
- National Institute of Standards and Technology, 325 Broadway, Boulder, CO 80305–3337, USA
- National Physical Laboratory (NPL), Teddington TW11 0LW, UK
| | - M. Sekido
- National Institute of Information and Communications Technology, 4-2-1 Nukuikitamachi, Koganei, 184-8795 Tokyo, Japan
| | - R. Le Targat
- LNE-SYRTE, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, 61 avenue de l’Observatoire 75014 Paris, France
| | - P. Wolf
- LNE-SYRTE, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, 61 avenue de l’Observatoire 75014 Paris, France
| | - X. Zhang
- National Institute of Standards and Technology, 325 Broadway, Boulder, CO 80305–3337, USA
| | - B. Zjawin
- Institute of Physics, Faculty of Physics, Astronomy and Informatics, Nicolaus Copernicus University, Grudziądzka 5, PL-87-100 Toruń, Poland
| | - M. Zawada
- Institute of Physics, Faculty of Physics, Astronomy and Informatics, Nicolaus Copernicus University, Grudziądzka 5, PL-87-100 Toruń, Poland
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Safronova MS, Porsev SG, Sanner C, Ye J. Two Clock Transitions in Neutral Yb for the Highest Sensitivity to Variations of the Fine-Structure Constant. Phys Rev Lett 2018; 120:173001. [PMID: 29756836 DOI: 10.1103/physrevlett.120.173001] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/18/2018] [Revised: 03/07/2018] [Indexed: 06/08/2023]
Abstract
We propose a new frequency standard based on a 4f^{14}6s6p ^{3}P_{0}-4f^{13}6s^{2}5d (J=2) transition in neutral Yb. This transition has a potential for high stability and accuracy and the advantage of the highest sensitivity among atomic clocks to variation of the fine-structure constant α. We find its dimensionless α-variation enhancement factor to be K=-15, in comparison to the most sensitive current clock (Yb^{+} E3, K=-6), and it is 18 times larger than in any neutral-atomic clocks (Hg, K=0.8). Combined with the unprecedented stability of an optical lattice clock for neutral atoms, this high sensitivity opens new perspectives for searches for ultralight dark matter and for tests of theories beyond the standard model of elementary particles. Moreover, together with the well-established ^{1}S_{0}-^{3}P_{0} transition, one will have two clock transitions operating in neutral Yb, whose interleaved interrogations may further reduce systematic uncertainties of such clock-comparison experiments.
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Affiliation(s)
- Marianna S Safronova
- Department of Physics and Astronomy, University of Delaware, Newark, Delaware 19716, USA
- Joint Quantum Institute, National Institute of Standards and Technology and the University of Maryland, College Park, Maryland 20742, USA
| | - Sergey G Porsev
- Department of Physics and Astronomy, University of Delaware, Newark, Delaware 19716, USA
- Petersburg Nuclear Physics Institute of NRC "Kurchatov Institute", Gatchina 188300, Russia
| | - Christian Sanner
- JILA, NIST and University of Colorado, Boulder, Colorado 80309, USA and Department of Physics, University of Colorado, Boulder, Colorado 80309, USA
| | - Jun Ye
- JILA, NIST and University of Colorado, Boulder, Colorado 80309, USA and Department of Physics, University of Colorado, Boulder, Colorado 80309, USA
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Kanekar N, Ghosh T, Chengalur JN. Stringent Constraints on Fundamental Constant Evolution Using Conjugate 18 cm Satellite OH Lines. Phys Rev Lett 2018; 120:061302. [PMID: 29481221 DOI: 10.1103/physrevlett.120.061302] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 08/15/2017] [Revised: 11/23/2017] [Indexed: 06/08/2023]
Abstract
We have used the Arecibo Telescope to carry out one of the deepest-ever integrations in radio astronomy, targeting the redshifted conjugate satellite OH 18 cm lines at z≈0.247 towards PKS 1413+135. The satellite OH 1720 and 1612 MHz lines are, respectively, in emission and absorption, with exactly the same line shapes due to population inversion in the OH ground state levels. Since the 1720 and 1612 MHz line rest frequencies have different dependences on the fine structure constant α and the proton-electron mass ratio μ, a comparison between their measured redshifts allows one to probe changes in α and μ with cosmological time. In the case of conjugate satellite OH 18 cm lines, the predicted perfect cancellation of the sum of the line optical depths provides a strong test for the presence of systematic effects that might limit their use in probing fundamental constant evolution. A nonparametric analysis of our new Arecibo data yields [ΔX/X]=(+0.97±1.52)×10^{-6}, where X≡μα^{2}. Combining this with our earlier results from the Arecibo Telescope and the Westerbork Synthesis Radio Telescope, we obtain [ΔX/X]=(-1.0±1.3)×10^{-6}, consistent with no changes in the quantity μα^{2} over the last 2.9 Gyr. This is the most stringent present constraint on fractional changes in μα^{2} from astronomical spectroscopy, and with no evidence for systematic effects.
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Affiliation(s)
- Nissim Kanekar
- National Centre for Radio Astrophysics, Pune 411 007, India
| | - Tapasi Ghosh
- Arecibo Observatory, Arecibo, Puerto Rico 00612, USA
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Abstract
The observational evidence for the recent acceleration of the universe demonstrates that canonical theories of cosmology and particle physics are incomplete-if not incorrect-and that new physics is out there, waiting to be discovered. A key task for the next generation of laboratory and astrophysical facilities is to search for, identify and ultimately characterize this new physics. Here we highlight recent developments in tests of the stability of nature's fundamental couplings, which provide a direct handle on new physics: a detection of variations will be revolutionary, but even improved null results provide competitive constraints on a range of cosmological and particle physics paradigms. A joint analysis of all currently available data shows a preference for variations of α and μ at about the two-sigma level, but inconsistencies between different sub-sets (likely due to hidden systematics) suggest that these statistical preferences need to be taken with caution. On the other hand, these measurements strongly constrain Weak Equivalence Principle violations. Plans and forecasts for forthcoming studies with facilities such as ALMA, ESPRESSO and the ELT, which should clarify these issues, are also discussed, and synergies with other probes are briefly highlighted. The goal is to show how a new generation of precision consistency tests of the standard paradigm will soon become possible.
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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, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal
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Abstract
Two new high-precision measurements of the deuterium abundance from absorbers along the line of sight to the quasar PKS1937–1009 were presented. The absorbers have lower neutral hydrogen column densities (N(HI) ≈ 18 cm − 2 ) than for previous high-precision measurements, boding well for further extensions of the sample due to the plenitude of low column density absorbers. The total high-precision sample now consists of 12 measurements with a weighted average deuterium abundance of D/H = 2 . 55 ± 0 . 02 × 10 − 5 . The sample does not favour a dipole similar to the one detected for the fine structure constant. The increased precision also calls for improved nucleosynthesis predictions. For that purpose we have updated the public AlterBBN code including new reactions, updated nuclear reaction rates, and the possibility of adding new physics such as dark matter. The standard Big Bang Nucleosynthesis prediction of D/H = 2 . 456 ± 0 . 057 × 10 − 5 is consistent with the observed value within 1.7 standard deviations.
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Leite A, Martins C, Molaro P. Dark Energy Constraints from Espresso Tests of the Stability of Fundamental Couplings. Universe 2017; 3:30. [DOI: 10.3390/universe3020030] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
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Abstract
Future cosmological surveys will probe the expansion history of the Universe and constrain phenomenological models of dark energy. Such models do not address the fine-tuning problem of the vacuum energy, i.e., the cosmological constant problem (CCP), but can make it spectacularly worse. We show that this is the case for "interacting dark energy" models in which the masses of the dark matter states depend on the dark energy sector. If realized in nature, these models have far-reaching implications for proposed solutions to the CCP that require the number of vacua to exceed the fine-tuning of the vacuum energy density. We show that current estimates of the number of flux vacua in string theory, N_{vac}∼O(10^{272 000}), are far too small to realize certain simple models of interacting dark energy and solve the cosmological constant problem anthropically. These models admit distinctive observational signatures that can be targeted by future gamma-ray observatories, hence making it possible to observationally rule out the anthropic solution to the cosmological constant problem in theories with a finite number of vacua.
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Affiliation(s)
- M C David Marsh
- Department of Applied Mathematics and Theoretical Physics, University of Cambridge, Cambridge CB3 0WA, United Kingdom
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Leefer N, Gerhardus A, Budker D, Flambaum VV, Stadnik YV. Search for the Effect of Massive Bodies on Atomic Spectra and Constraints on Yukawa-Type Interactions of Scalar Particles. Phys Rev Lett 2016; 117:271601. [PMID: 28084774 DOI: 10.1103/physrevlett.117.271601] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/25/2016] [Indexed: 06/06/2023]
Abstract
We propose a new method to search for hypothetical scalar particles that have feeble interactions with standard-model particles. In the presence of massive bodies, these interactions produce a nonzero Yukawa-type scalar-field magnitude. Using radio-frequency spectroscopy data of atomic dysprosium, as well as atomic clock spectroscopy data, we constrain the Yukawa-type interactions of a scalar field with the photon, electron, and nucleons for a range of scalar-particle masses corresponding to length scales >10 cm. In the limit as the scalar-particle mass m_{ϕ}→0, our derived limits on the Yukawa-type interaction parameters are Λ_{γ}≳8×10^{19} GeV, Λ_{e}≳1.3×10^{19} GeV, and Λ_{N}≳6×10^{20} GeV. Our measurements also constrain combinations of interaction parameters, which cannot otherwise be probed with traditional anomalous-force measurements. We suggest further measurements to improve on the current level of sensitivity.
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Affiliation(s)
- N Leefer
- Helmholtz-Institut Mainz, Johannes Gutenberg-Universitat Mainz, 55128 Mainz, Germany
| | - A Gerhardus
- Bethe Center for Theoretical Physics, Physikalisches Institut der Universitat Bonn, 53115 Bonn, Germany
| | - D Budker
- Helmholtz-Institut Mainz, Johannes Gutenberg-Universitat Mainz, 55128 Mainz, Germany
- Physics Department, University of California, Berkeley 94720-7300, USA
- Nuclear Science Division, Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA
| | - V V Flambaum
- Helmholtz-Institut Mainz, Johannes Gutenberg-Universitat Mainz, 55128 Mainz, Germany
- School of Physics, University of New South Wales, Sydney 2052, Australia
| | - Y V Stadnik
- School of Physics, University of New South Wales, Sydney 2052, Australia
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De Martino I, Martins C, Ebeling H, Kocevski D. New Constraints on Spatial Variations of the Fine Structure Constant from Clusters of Galaxies. Universe 2016; 2:34. [DOI: 10.3390/universe2040034] [Citation(s) in RCA: 8] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/17/2022]
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Daprà M, Niu ML, Salumbides EJ, Murphy MT, Ubachs W. CONSTRAINT ON A COSMOLOGICAL VARIATION IN THE PROTON-TO-ELECTRON MASS RATIO FROM ELECTRONIC CO ABSORPTION. ACTA ACUST UNITED AC 2016; 826:192. [DOI: 10.3847/0004-637x/826/2/192] [Citation(s) in RCA: 21] [Impact Index Per Article: 2.6] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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Martins C, Pinho A, Carreira P, Gusart A, López J, Rocha C. Fine-structure constant constraints on dark energy. II. Extending the parameter space. Int J Clin Exp Med 2016. [DOI: 10.1103/physrevd.93.023506] [Citation(s) in RCA: 16] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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Schmöger L, Schwarz M, Baumann TM, Versolato OO, Piest B, Pfeifer T, Ullrich J, Schmidt PO, López-Urrutia JRC. Deceleration, precooling, and multi-pass stopping of highly charged ions in Be⁺ Coulomb crystals. Rev Sci Instrum 2015; 86:103111. [PMID: 26520944 DOI: 10.1063/1.4934245] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/05/2023]
Abstract
Preparing highly charged ions (HCIs) in a cold and strongly localized state is of particular interest for frequency metrology and tests of possible spatial and temporal variations of the fine structure constant. Our versatile preparation technique is based on the generic modular combination of a pulsed ion source with a cryogenic linear Paul trap. Both instruments are connected by a compact beamline with deceleration and precooling properties. We present its design and commissioning experiments regarding these two functionalities. A pulsed buncher tube allows for the deceleration and longitudinal phase-space compression of the ion pulses. External injection of slow HCIs, specifically Ar(13+), into the linear Paul trap and their subsequent retrapping in the absence of sympathetic cooling is demonstrated. The latter proved to be a necessary prerequisite for the multi-pass stopping of HCIs in continuously laser-cooled Be(+) Coulomb crystals.
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Affiliation(s)
- L Schmöger
- Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany
| | - M Schwarz
- Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany
| | - T M Baumann
- Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany
| | - O O Versolato
- Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany
| | - B Piest
- Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany
| | - T Pfeifer
- Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany
| | - J Ullrich
- Physikalisch-Technische Bundesanstalt, Bundesallee 100, 38116 Braunschweig, Germany
| | - P O Schmidt
- Physikalisch-Technische Bundesanstalt, Bundesallee 100, 38116 Braunschweig, Germany
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Stadnik YV, Flambaum VV. Searching for dark matter and variation of fundamental constants with laser and maser interferometry. Phys Rev Lett 2015; 114:161301. [PMID: 25955044 DOI: 10.1103/physrevlett.114.161301] [Citation(s) in RCA: 11] [Impact Index Per Article: 1.2] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/16/2015] [Indexed: 06/04/2023]
Abstract
Any slight variations in the fundamental constants of nature, which may be induced by dark matter or some yet-to-be-discovered cosmic field, would characteristically alter the phase of a light beam inside an interferometer, which can be measured extremely precisely. Laser and maser interferometry may be applied to searches for the linear-in-time drift of the fundamental constants, detection of topological defect dark matter through transient-in-time effects, and for a relic, coherently oscillating condensate, which consists of scalar dark matter fields, through oscillating effects. Our proposed experiments require either minor or no modifications of existing apparatus, and offer extensive reach into important and unconstrained spaces of physical parameters.
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Affiliation(s)
- Y V Stadnik
- School of Physics, University of New South Wales, Sydney 2052, Australia
| | - V V Flambaum
- School of Physics, University of New South Wales, Sydney 2052, Australia
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Windberger A, Crespo López-Urrutia JR, Bekker H, Oreshkina NS, Berengut JC, Bock V, Borschevsky A, Dzuba VA, Eliav E, Harman Z, Kaldor U, Kaul S, Safronova UI, Flambaum VV, Keitel CH, Schmidt PO, Ullrich J, Versolato OO. Identification of the predicted 5s-4f level crossing optical lines with applications to metrology and searches for the variation of fundamental constants. Phys Rev Lett 2015; 114:150801. [PMID: 25933300 DOI: 10.1103/physrevlett.114.150801] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/09/2015] [Indexed: 06/04/2023]
Abstract
We measure optical spectra of Nd-like W, Re, Os, Ir, and Pt ions of particular interest for studies of a possibly varying fine-structure constant. Exploiting characteristic energy scalings we identify the strongest lines, confirm the predicted 5s-4f level crossing, and benchmark advanced calculations. We infer two possible values for optical M2/E3 and E1 transitions in Ir^{17+} that have the highest predicted sensitivity to a variation of the fine-structure constant among stable atomic systems. Furthermore, we determine the energies of proposed frequency standards in Hf^{12+} and W^{14+}.
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Affiliation(s)
- A Windberger
- Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany
| | | | - H Bekker
- Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany
| | - N S Oreshkina
- Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany
| | - J C Berengut
- School of Physics, University of New South Wales, Sydney, New South Wales 2052, Australia
| | - V Bock
- Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany
| | - A Borschevsky
- Centre for Theoretical Chemistry and Physics, The New Zealand Institute for Advanced Study, Massey University Auckland, Private Bag 102904, 0745 Auckland, New Zealand
| | - V A Dzuba
- School of Physics, University of New South Wales, Sydney, New South Wales 2052, Australia
| | - E Eliav
- School of Chemistry, Tel Aviv University, 69978 Tel Aviv, Israel
| | - Z Harman
- Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany
| | - U Kaldor
- School of Chemistry, Tel Aviv University, 69978 Tel Aviv, Israel
| | - S Kaul
- Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany
| | - U I Safronova
- Physics Department, University of Nevada, Reno, Nevada 89557, USA
| | - V V Flambaum
- School of Physics, University of New South Wales, Sydney, New South Wales 2052, Australia
| | - C H Keitel
- Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany
| | - P O Schmidt
- Physikalisch-Technische Bundesanstalt, Bundesallee 100, 38116 Braunschweig, Germany
- Institut für Quantenoptik, Leibniz Universität Hannover, Welfengarten 1, 30167 Hannover, Germany
| | - J Ullrich
- Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany
- Physikalisch-Technische Bundesanstalt, Bundesallee 100, 38116 Braunschweig, Germany
| | - O O Versolato
- Physikalisch-Technische Bundesanstalt, Bundesallee 100, 38116 Braunschweig, Germany
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Dzuba VA, Flambaum VV. Highly charged ions for atomic clocks and search for variation of the fine structure constant. ACTA ACUST UNITED AC 2015; 236:79-86. [DOI: 10.1007/s10751-015-1166-4] [Citation(s) in RCA: 8] [Impact Index Per Article: 0.9] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 10/23/2022]
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Abstract
In this Letter, we describe a new method to use baryon acoustic oscillations (BAO) to derive a constraint on the possible variation of the speed of light. The method relies on the fact that there is a simple relation between the angular diameter distance (D(A)) maximum and the Hubble function (H) evaluated at the same maximum-condition redshift, which includes speed of light c. We note the close analogy of the BAO probe with a laboratory experiment: here we have D(A) which plays the role of a standard (cosmological) ruler, and H^{-1}, with the dimension of time, as a (cosmological) clock. We evaluate if current or future missions such as Euclid can be sensitive enough to detect any variation of c.
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Affiliation(s)
- Vincenzo Salzano
- Institute of Physics, University of Szczecin, Wielkopolska 15, 70-451 Szczecin, Poland
| | - Mariusz P Dąbrowski
- Institute of Physics, University of Szczecin, Wielkopolska 15, 70-451 Szczecin, Poland
- Copernicus Center for Interdisciplinary Studies, Sławkowska 17, 31-016 Kraków, Poland
| | - Ruth Lazkoz
- Fisika Teorikoaren eta Zientziaren Historia Saila, Zientzia eta Teknologia Fakultatea, Euskal Herriko Unibertsitatea, 644 Posta Kutxatila, 48080 Bilbao, Spain
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Godun RM, Nisbet-Jones PBR, Jones JM, King SA, Johnson LAM, Margolis HS, Szymaniec K, Lea SN, Bongs K, Gill P. Frequency ratio of two optical clock transitions in 171Yb+ and constraints on the time variation of fundamental constants. Phys Rev Lett 2014; 113:210801. [PMID: 25479482 DOI: 10.1103/physrevlett.113.210801] [Citation(s) in RCA: 81] [Impact Index Per Article: 8.1] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/30/2014] [Indexed: 06/04/2023]
Abstract
Singly ionized ytterbium, with ultranarrow optical clock transitions at 467 and 436 nm, is a convenient system for the realization of optical atomic clocks and tests of present-day variation of fundamental constants. We present the first direct measurement of the frequency ratio of these two clock transitions, without reference to a cesium primary standard, and using the same single ion of 171Yb+. The absolute frequencies of both transitions are also presented, each with a relative standard uncertainty of 6×10(-16). Combining our results with those from other experiments, we report a threefold improvement in the constraint on the time variation of the proton-to-electron mass ratio, μ/μ=0.2(1.1)×10(-16) yr(-1), along with an improved constraint on time variation of the fine structure constant, α/α=-0.7(2.1)×10(-17) yr(-1).
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Affiliation(s)
- R M Godun
- National Physical Laboratory, Hampton Road, Teddington TW11 0LW, United Kingdom
| | - P B R Nisbet-Jones
- National Physical Laboratory, Hampton Road, Teddington TW11 0LW, United Kingdom
| | - J M Jones
- National Physical Laboratory, Hampton Road, Teddington TW11 0LW, United Kingdom and School of Physics and Astronomy, University of Birmingham, Birmingham B15 2TT, United Kingdom
| | - S A King
- National Physical Laboratory, Hampton Road, Teddington TW11 0LW, United Kingdom
| | - L A M Johnson
- National Physical Laboratory, Hampton Road, Teddington TW11 0LW, United Kingdom
| | - H S Margolis
- National Physical Laboratory, Hampton Road, Teddington TW11 0LW, United Kingdom
| | - K Szymaniec
- National Physical Laboratory, Hampton Road, Teddington TW11 0LW, United Kingdom
| | - S N Lea
- National Physical Laboratory, Hampton Road, Teddington TW11 0LW, United Kingdom
| | - K Bongs
- School of Physics and Astronomy, University of Birmingham, Birmingham B15 2TT, United Kingdom
| | - P Gill
- National Physical Laboratory, Hampton Road, Teddington TW11 0LW, United Kingdom
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Huntemann N, Lipphardt B, Tamm C, Gerginov V, Weyers S, Peik E. Improved limit on a temporal variation of mp/me from comparisons of Yb+ and Cs atomic clocks. Phys Rev Lett 2014; 113:210802. [PMID: 25479483 DOI: 10.1103/physrevlett.113.210802] [Citation(s) in RCA: 20] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/16/2014] [Indexed: 06/04/2023]
Abstract
Accurate measurements of different transition frequencies between atomic levels of the electronic and hyperfine structure over time are used to investigate temporal variations of the fine structure constant α and the proton-to-electron mass ratio μ. We measure the frequency of the (2)S1/2→(2)F7/2 electric octupole (E3) transition in (171)Yb(+) against two caesium fountain clocks as f(E3)=642,121,496,772,645.36 Hz with an improved fractional uncertainty of 3.9×10(-16). This transition frequency shows a strong sensitivity to changes of α. Together with a number of previous and recent measurements of the (2)S1/2→(2)D3/2 electric quadrupole transition in (171)Yb(+) and with data from other elements, a least-squares analysis yields (1/α)(dα/dt)=-0.20(20)×10(-16)/yr and (1/μ)(dμ/dt)=-0.5(1.6)×10(-16)/yr, confirming a previous limit on dα/dt and providing the most stringent limit on dμ/dt from laboratory experiments.
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Affiliation(s)
- N Huntemann
- Physikalisch-Technische Bundesanstalt, Bundesallee 100, 38116 Braunschweig, Germany
| | - B Lipphardt
- Physikalisch-Technische Bundesanstalt, Bundesallee 100, 38116 Braunschweig, Germany
| | - Chr Tamm
- Physikalisch-Technische Bundesanstalt, Bundesallee 100, 38116 Braunschweig, Germany
| | - V Gerginov
- Physikalisch-Technische Bundesanstalt, Bundesallee 100, 38116 Braunschweig, Germany
| | - S Weyers
- Physikalisch-Technische Bundesanstalt, Bundesallee 100, 38116 Braunschweig, Germany
| | - E Peik
- Physikalisch-Technische Bundesanstalt, Bundesallee 100, 38116 Braunschweig, Germany
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Bagdonaite J, Salumbides EJ, Preval SP, Barstow MA, Barrow JD, Murphy MT, Ubachs W. Limits on a gravitational field dependence of the proton-electron mass ratio from H2 in white dwarf stars. Phys Rev Lett 2014; 113:123002. [PMID: 25279624 DOI: 10.1103/physrevlett.113.123002] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/03/2014] [Indexed: 06/03/2023]
Abstract
Spectra of molecular hydrogen (H2) are employed to search for a possible proton-to-electron mass ratio (μ) dependence on gravity. The Lyman transitions of H2, observed with the Hubble Space Telescope towards white dwarf stars that underwent a gravitational collapse, are compared to accurate laboratory spectra taking into account the high temperature conditions (T∼13 000 K) of their photospheres. We derive sensitivity coefficients Ki which define how the individual H2 transitions shift due to μ dependence. The spectrum of white dwarf star GD133 yields a Δμ/μ constraint of (-2.7±4.7stat±0.2syst)×10(-5) for a local environment of a gravitational potential ϕ∼10(4) ϕEarth, while that of G29-38 yields Δμ/μ=(-5.8±3.8stat±0.3syst)×10(-5) for a potential of 2×10(4) ϕEarth.
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Affiliation(s)
- J Bagdonaite
- Department of Physics and Astronomy, and LaserLaB, VU University, De Boelelaan 1081, 1081 HV Amsterdam, Netherlands
| | - E J Salumbides
- Department of Physics and Astronomy, and LaserLaB, VU University, De Boelelaan 1081, 1081 HV Amsterdam, Netherlands and Department of Physics, University of San Carlos, Cebu City 6000, Philippines
| | - S P Preval
- Department of Physics and Astronomy, University of Leicester, University Road, Leicester LEI 7RH, United Kingdom
| | - M A Barstow
- Department of Physics and Astronomy, University of Leicester, University Road, Leicester LEI 7RH, United Kingdom
| | - J D Barrow
- DAMTP, Centre for Mathematical Sciences, University of Cambridge, Cambridge CB3 0WA, United Kingdom
| | - M T Murphy
- Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Melbourne, Victoria 3122, Australia
| | - W Ubachs
- Department of Physics and Astronomy, and LaserLaB, VU University, De Boelelaan 1081, 1081 HV Amsterdam, Netherlands
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Safronova MS, Dzuba VA, Flambaum VV, Safronova UI, Porsev SG, Kozlov MG. Highly charged ions for atomic clocks, quantum information, and search for α variation. Phys Rev Lett 2014; 113:030801. [PMID: 25083627 DOI: 10.1103/physrevlett.113.030801] [Citation(s) in RCA: 6] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/16/2014] [Indexed: 06/03/2023]
Abstract
We propose 10 highly charged ions as candidates for the development of next generation atomic clocks, quantum information, and search for α variation. They have long-lived metastable states with transition wavelengths to the ground state between 170-3000 nm, relatively simple electronic structure, stable isotopes, and high sensitivity to α variation (e.g., Sm(14+), Pr(10+), Sm(13+), Nd(10+)). We predict their properties crucial for the experimental exploration and highlight particularly attractive systems for these applications.
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Affiliation(s)
- M S Safronova
- University of Delaware, Newark, Delaware 19716, USA and Joint Quantum Institute, NIST and the University of Maryland, College Park, Maryland 20899, USA
| | - V A Dzuba
- The University of New South Wales, Sydney 2052, Australia
| | - V V Flambaum
- The University of New South Wales, Sydney 2052, Australia
| | - U I Safronova
- University of Nevada, Reno, Nevada 89557, USA and University of Notre Dame, Notre Dame, Indiana 46556, USA
| | - S G Porsev
- University of Delaware, Newark, Delaware 19716, USA and Petersburg Nuclear Physics Institute, Gatchina 188300, Russia
| | - M G Kozlov
- Petersburg Nuclear Physics Institute, Gatchina 188300, Russia and St. Petersburg Electrotechnical University "LETI," St. Petersburg 197376, Russia
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