Fundamental constants: from measurement to the universe, a window on gravitation and cosmology

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Abstract Fundamental constants are a cornerstone of our physical laws. Any constant varying in space and/or time would signal a violation of local position invariance and be associated with a violation of the universality of free fall, and hence of the weak equivalence principle at the heart of the geometrisation of gravity. It will also reflect the existence of new degrees of freedom that couple to standard matter fields. Thus, testing for the stability of fundamental constants is of utmost importance for our understanding of gravity and for characterizing the domain of validity of general relativity. Besides, it opens an independent window on the dark matter and dark energy components. As a consequence, thanks to the active developments of experiments, fundamental constants have become a key player in our search for physics beyond the standard model of particle physics and general relativity. This review details the various roles of the fundamental constants in the laws of physics and in the construction of the international system of units, which now depends strongly on them. This requires to distinguish the concepts of fundamental units and fundamental parameters. Then, the relations between constants, the tests of the local position invariance and of the universality of free fall are presented, as well as the construction of field theories that account for “varying constants” and the motivations arising from high-energy physics and string theory. From a theoretical perspective any varying fundamental parameter is related to a dynamical field, the dynamics of which is dictated from the whole theory so that it remains fully consistent: no arbitrary law of variation has to be postulated. Then, the main experimental and observational constraints that have been obtained from atomic clocks, the Oklo phenomenon, solar system observations, meteorite dating, quasar absorption spectra, stellar physics, pulsar timing, the cosmic microwave background and Big Bang nucleosynthesis are described. It details the basics of each system, its dependence with respect to the primary parameters the variation of which can be constrained from observations, the known systematic effects and the most recent constraints. It also describes how these primary parameters can be related to the fundamental constants and the model-dependencies that is involved. Both time and space variations are considered. To finish, it contains a short discussion on the more speculative possibility of understanding the numerical values of the fundamental parameters in view of the apparent fine-tuning that they confront us with, by invoking anthropic arguments. Given the huge increase of data and constraints and the difficulty to standardize them, a general scheme to present experimental and observational results and to construct a collaborative data base that will be more efficient for the community and allow us for better traceability, is proposed.

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Varying Constants, Gravitation and Cosmology.
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  • Jean-Philippe Uzan

Fundamental constants are a cornerstone of our physical laws. Any constant varying in space and/or time would reflect the existence of an almost massless field that couples to matter. This will induce a violation of the universality of free fall. Thus, it is of utmost importance for our understanding of gravity and of the domain of validity of general relativity to test for their constancy. We detail the relations between the constants, the tests of the local position invariance and of the universality of free fall. We then review the main experimental and observational constraints that have been obtained from atomic clocks, the Oklo phenomenon, solar system observations, meteorite dating, quasar absorption spectra, stellar physics, pulsar timing, the cosmic microwave background and big bang nucleosynthesis. At each step we describe the basics of each system, its dependence with respect to the constants, the known systematic effects and the most recent constraints that have been obtained. We then describe the main theoretical frameworks in which the low-energy constants may actually be varying and we focus on the unification mechanisms and the relations between the variation of different constants. To finish, we discuss the more speculative possibility of understanding their numerical values and the apparent fine-tuning that they confront us with.

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Temporal and spatial variation of fundamental constants: theory and observations
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Space-time variation of the fundamental constants is suggested by theories unifying gravity with other interactions. It also can explain fine tuning of the fundamental constants which is needed for life to appear. Review of recent works devoted to the variation of the fine structure constant a, strong interaction and fundamental masses (Higgs vacuum) is presented. The results from Big Bang nucleosynthesis, quasar absorption spectra, and Oklo natural nuclear reactor data give us the space-time variation on the Universe lifetime scale. Comparison of different atomic clocks gives us the present time variation. Assuming linear variation with time we can compare different results. The best limit on the variation of the electron-to-proton mass ratio mu = m <sub xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xlink="http://www.w3.org/1999/xlink">e</sub> /M <sub xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xlink="http://www.w3.org/1999/xlink">p</sub> and X <sub xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xlink="http://www.w3.org/1999/xlink">e</sub> = m <sub xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xlink="http://www.w3.org/1999/xlink">e</sub> /Lambda <sub xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xlink="http://www.w3.org/1999/xlink">QCD</sub> follows from the quasar absorption spectra [1]: mu dot/mu = X dot <sub xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xlink="http://www.w3.org/1999/xlink">e</sub> /X <sub xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xlink="http://www.w3.org/1999/xlink">e</sub> = (1plusmn3) times 10 <sup xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xlink="http://www.w3.org/1999/xlink">-16</sup> yr <sup xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xlink="http://www.w3.org/1999/xlink">-1</sup> . A combination of this result and the atomic clock results [2, 3] gives the best Unit on variation of alpha: alpha dot/alpha = (-0.8 plusmn 0.8) times 10 <sup xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xlink="http://www.w3.org/1999/xlink">-16</sup> yr <sup xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xlink="http://www.w3.org/1999/xlink">-1</sup> . The Oklo natural reactor gives the best limit on the variation of X <sub xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xlink="http://www.w3.org/1999/xlink">s</sub> = m <sub xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xlink="http://www.w3.org/1999/xlink">s</sub> /Lambda <sub xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xlink="http://www.w3.org/1999/xlink">QCD</sub> where m <sub xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xlink="http://www.w3.org/1999/xlink">s</sub> is the strange quark mass [4, 5]: |X dot <sub xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xlink="http://www.w3.org/1999/xlink">s</sub> /X <sub xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xlink="http://www.w3.org/1999/xlink">s</sub> | < 10 <sup xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xlink="http://www.w3.org/1999/xlink">-18</sup> yr <sup xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xlink="http://www.w3.org/1999/xlink">-1</sup> . Note that the Oklo data can not give us any limit on the variation of alpha since the effect of alpha there is much smaller than the effect of X <sub xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xlink="http://www.w3.org/1999/xlink">s</sub> and should be neglected. Huge enhancement of the relative variation effects happens in transitions between close atomic, molecular and nuclear energy levels. We suggest several new cases where the levels are very narrow. Large enhancement of the variation effects is also possible in cold atomic and molecular collisions near Feshbach resonance. How changing physical constants and violation of local position invariance may occur? Light scalar fields very naturally appear in modern cosmological models, affecting parameters of the standard model (e.g. alpha). 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The strongest limits [6] kalpha + 0.17k <sub xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xlink="http://www.w3.org/1999/xlink">e</sub> = (-3.5 plusmn 6) times 10 <sup xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xlink="http://www.w3.org/1999/xlink">-7</sup> and k <sub xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xlink="http://www.w3.org/1999/xlink">alpha</sub> + 0.13k <sub xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xlink="http://www.w3.org/1999/xlink">q</sub> = (-1 plusmn 17) times 10 <sup xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xlink="http://www.w3.org/1999/xlink">-7</sup> are obtained from the measurements of dependence of atomic frequencies on the distance from Sun [2, 7] (the distance varies due to the ellipticity of the Earth's orbit).

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Review of recent works devoted to the variation of the fine structure constant α, strong interaction and fundamental masses (Higgs vacuum) is presented. The results from Big Bang nucleosynthesis, quasar absorption spectra, and Oklo natural nuclear reactor data give us the space-time variation on the Universe lifetime scale. Comparison of different atomic clocks gives us the present time variation. Assuming linear variation with time we can compare different results. The best limit on the variation of the electron-to-proton mass ratio μ = me/Mp and Xe = me/ΛQCD follows from the quasar absorption spectra:1[Formula: see text]. A combination of this result and the atomic clock results2,3 gives the best limt on variation of [Formula: see text]. The Oklo natural reactor gives the best limit on the variation of Xs = ms/ΛQCD where ms is the strange quark mass:4,5[Formula: see text]. Note that the Oklo data can not give us any limit on the variation of α since the effect of α there is much smaller than the effect of Xs and should be neglected. Huge enhancement of the relative variation effects happens in transitions between close atomic, molecular and nuclear energy levels. We suggest several new cases where the levels are very narrow. Large enhancement of the variation effects is also possible in cold atomic and molecular collisions near Feshbach resonance. How changing physical constants and violation of local position invariance may occur? Light scalar fields very naturally appear in modern cosmological models, affecting parameters of the Standard Model (e.g. α). Cosmological variations of these scalar fields should occur because of drastic changes of matter composition in Universe: the latest such event is rather recent (about 5 billion years ago), from matter to dark energy domination. Massive bodies (stars or galaxies) can also affect physical constants. They have large scalar charge S proportional to number of particles which produces a Coulomb-like scalar field U = S/r. This leads to a variation of the fundamental constants proportional to the gravitational potential, e.g. δα/α = kαδ(GM/rc2). We compare different manifestations of this effect. The strongest limits6kα + 0.17ke = (-3.5 ±6) × 10-7 and kα + 0.13kq = (-1 ± 17) × 10-7 are obtained from the measurements of dependence of atomic frequencies on the distance from Sun2,7 (the distance varies due to the ellipticity of the Earth's orbit).

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BBN and the CMB constrain neutrino coupled light WIMPs
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Probing Physics Beyond the Standard Model: Limits from BBN and the CMB Independently and Combined
  • Jul 26, 2022
  • arXiv (Cornell University)
  • Tsung-Han Yeh + 3 more

We present new Big Bang Nucleosynthesis (BBN) limits on the cosmic expansion rate or relativistic energy density, quantified via the number $N_\nu$ of equivalent neutrino species. We use the latest light element observations, neutron mean lifetime, and update our evaluation for the nuclear rates $d+d \rightarrow He3 + n$ and $d+d \rightarrow H3 + p$. Combining this result with the independent constraints from the cosmic microwave background (CMB) yields tight limits on new physics that perturbs $N_\nu$ and $\eta$ prior to cosmic nucleosynthesis: a joint BBN+CMB analysis gives $N_\nu = 2.898 \pm 0.141$, resulting in $N_\nu < 3.180$ at $2\sigma$. We apply these limits to a wide variety of new physics scenarios including right-handed neutrinos, dark radiation, and a stochastic gravitational wave background. We also search for limits on potential {\em changes} in $N_\nu$ and/or the baryon-to-photon ratio $\eta$ between the two epochs. The present data place strong constraints on the allowed changes in $N_\nu$ between BBN and CMB decoupling; for example, we find $-0.708 < N_\nu^{\rm CMB}-N_\nu^{\rm BBN} < 0.328$ in the case where $\eta$ and the primordial helium mass fraction $Y_p$ are unchanged between the two epochs; we also give limits on the allowed variations in $\eta$ or in $(\eta,N_\nu)$ jointly. Looking to the future, we forecast the tightened precision for $N_\nu$ arising from both CMB Stage 4 measurements as well as improvements in astronomical \he4 measurements. We find that CMB-S4 combined with present BBN and light element observation precision can give $\sigma(N_\nu) \simeq 0.03$. Such future precision would reveal the expected effect of neutrino heating ($N_{\rm eff}-3=0.044$) of the CMB during BBN, and would be near the level to reveal any particle species ever in thermal equilibrium with the standard model.

  • Conference Article
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  • 10.1063/1.2915601
How changing physical constants and violation of local position invariance may occur?
  • Jan 1, 2008
  • V V Flambaum + 4 more

Light scalar fields very naturally appear in modern cosmological models, affecting such parameters of Standard Model as electromagnetic fine structure constant α, dimensionless ratios of electron or quark mass to the QCD scale, me,q/ΛQCD. Cosmological variations of these scalar fields should occur because of drastic changes of matter composition in Universe: the latest such event is rather recent (redshift z∼0.5), from matter to dark energy domination. In a two‐brane model (we use as a pedagogical example) these modifications are due to changing distance to “the second brane”, a massive companion of “our brane”. Back from extra dimensions, massive bodies (stars or galaxies) can also affect physical constants. They have large scalar charge Qd proportional to number of particles which produces a Coulomb‐like scalar field φ = Qd/r. This leads to a variation of the fundamental constants proportional to the gravitational potential, e.g. δα/α = kαδ(GM/rc2). We compare different manifestations of this effect, which is usually called violation of local position invariance. The strongest limits kα+0.17ke = (−3.5±6)*10−7 are obtained from the measurements of dependence of atomic frequencies on the distance from Sun (the distance varies due to the ellipticity of the Earth's orbit).

  • Research Article
  • Cite Count Icon 17
  • 10.1103/physrevd.69.103503
Precision primordial4Hemeasurement from the CMB
  • May 12, 2004
  • Physical Review D
  • Greg Huey + 2 more

Big bang nucleosynthesis (BBN) and the cosmic microwave background (CMB) are two major pillars of cosmology. Standard BBN accurately predicts the primordial light element abundances ${(}^{4}\mathrm{He},$ D, ${}^{3}\mathrm{He}$ and ${}^{7}\mathrm{Li}),$ depending on one parameter, the baryon density. Light element observations are used as a baryometer. The CMB anisotropies also contain information about the content of the Universe which allows an important consistency check on the big bang model. In addition CMB observations now have sufficient accuracy to not only determine the total baryon density, but also resolve its principal constituents H and ${}^{4}\mathrm{He}.$ We present a global analysis of all recent CMB data, with special emphasis on the concordance with BBN theory and light element observations. We find ${\ensuremath{\Omega}}_{B}{h}^{2}{=0.0250}_{\ensuremath{-}0.0026}^{+0.0019}$ and ${Y}_{p}{=0.250}_{\ensuremath{-}0.014}^{+0.010}$ (fraction of baryon mass as ${}^{4}\mathrm{He})$ using CMB data alone, in agreement with ${}^{4}\mathrm{He}$ abundance observations. The determination of ${Y}_{p}$ allows us to constrain the relativistic degrees of freedom during BBN, measured through the effective number of light neutrino species, ${N}_{\ensuremath{\nu},eff}{=3.02}_{\ensuremath{-}0.79}^{+0.85},$ in accord with the standard model of particle physics. With this concordance established we show that the inclusion of standard, ${N}_{\ensuremath{\nu},eff}\ensuremath{\equiv}3,$ BBN theory priors significantly reduces the volume of parameter space. In this case, we find ${\ensuremath{\Omega}}_{B}{h}^{2}{=0.0245}_{\ensuremath{-}0.0028}^{+0.0015}$ and ${Y}_{p}{=0.2493}_{\ensuremath{-}0.0010}^{+0.0007}.$ We also find that the inclusion of deuterium abundance observations reduces the ${Y}_{p}$ and ${\ensuremath{\Omega}}_{B}{h}^{2}$ ranges by a factor of $\ensuremath{\sim}2.$ Further light element observations and CMB anisotropy experiments will refine this concordance and sharpen BBN and the CMB as tools for precision cosmology.

  • Conference Article
  • Cite Count Icon 4
  • 10.1063/1.2400630
Variation of Fundamental Constants
  • Jan 1, 2006
  • V V Flambaum

Theories unifying gravity with other interactions suggest temporal and spatial variation of the fundamental “constants” in expanding Universe. The spatial variation can explain a fine tuning of the fundamental constants which allows humans (and any life) to appear. We appeared in the area of the Universe where the values of the fundamental constants are consistent with our existence.We present a review of recent works devoted to the variation of the fine structure constant α, strong interaction and fundamental masses. There are some hints for the variation in quasar absorption spectra. Big Bang nucleosynthesis, and Oklo natural nuclear reactor data.A very promising method to search for the variation of the fundamental constants consists in comparison of different atomic clocks. Huge enhancement of the variation effects happens in transition between accidentally degenerate atomic and molecular energy levels. A new idea is to build a “nuclear” clock based on the ultraviolet transition between very low excited state and ground state in Thorium nucleus. This may allow to improve sensitivity to the variation up to 10 orders of magnitude!Huge enhancement of the variation effects is also possible in cold atomic and molecular collisions near Feshbach resonance.

  • Research Article
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Searching for space-time variation of the fine structure constant using QSO spectra: overview and future prospects
  • Nov 1, 2009
  • Proceedings of the International Astronomical Union
  • J C Berengut + 6 more

Current theories that seek to unify gravity with the other fundamental interactions suggest that spatial and temporal variation of fundamental constants is a possibility, or even a necessity, in an expanding Universe. Several studies have tried to probe the values of constants at earlier stages in the evolution of the Universe, using tools such as big-bang nucleosynthesis, the Oklo natural nuclear reactor, quasar absorption spectra, and atomic clocks (see, e.g. Flambaum &amp; Berengut (2009)).

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