Limits on cosmological variation of strong interaction and quark masses from big bang nucleosynthesis, cosmic, laboratory and Oklo data

Flambaum, V. V.; Shuryak, Edward

doi:10.1103/physrevd.65.103503

Cited by 85 publications

(114 citation statements)

References 40 publications

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“…In order to make such a connection, we make use of previous analyses relating the deuterium binding energy B D to fundamental constants. Using a potential model, the dependence of B D on the nucleon, σ-meson and ω-meson has been estimated (Flambaum & Shuryak 2002;Dmitriev & Flambaum 2003;Flambaum & Shuryak 2003;Dmitriev et al 2004;Coc et al 2007;Damour & Donoghue 2008). Furthermore, using the quark matrix elements for the nucleon, variations in B D can be related to variations in the light quark masses (particularly the strange quark) and thus to the corresponding quark Yukawa couplings and Higgs vev, v. The remaining sensitivity of B D to a dimensionful quantity is ascribed to the QCD scale Λ.…”

Section: Using the Deuterium Binding Energy As A Linkmentioning

confidence: 99%

“…Martins et al 2004;Stefanescu 2007;Nakashima et al 2008;Scóccola et al 2008) and from big bang nucleosynthesis (BBN) (z ∼ 10 10 ) (e.g. Kolb et al 1986;Campbell & Olive 1995;Bergström et al 1999;Nollett & Lopez 2002;Ichikawa & Kawasaki 2002;Flambaum & Shuryak 2002;Müller et al 2004;Ichikawa & Kawasaki 2004;Landau et al 2006;Coc et al 2007;Dent et al 2007). We refer to Uzan (2003Uzan ( , 2004Uzan ( , 2009b for recent reviews on this topic.…”

Section: Introductionmentioning

confidence: 99%

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Effects of the variation of fundamental constants on Population III stellar evolution

Ekström

Coc

Descouvemont

et al. 2010

A&A

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Aims. A variation of the fundamental constants is expected to affect the thermonuclear rates important for stellar nucleosynthesis. In particular, because of the very low resonant energies of 8 Be and 12 C, the triple α process is extremely sensitive to any such variations. Methods. Using a microscopic model for these nuclei, we derive the sensitivity of the Hoyle state to the nucleon-nucleon potential, thereby allowing for a change in the magnitude of the nuclear interaction. We follow the evolution of 15 and 60 M zero-metallicity stellar models, up to the end of core helium burning. These stars are assumed to be representative of the first, Population III stars. Results. We derive limits on the variation in the magnitude of the nuclear interaction and model dependent limits on the variation of the fine structure constant based on the calculated oxygen and carbon abundances resulting from helium burning. The requirement that some 12 C and 16 O be present at the end of the helium burning phase allows for permille limits on the change in the nuclear interaction and limits of the order of 10 −5 on the fine structure constant relevant at a cosmological redshift of z ∼ 15−20.

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Section: Using the Deuterium Binding Energy As A Linkmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Effects of the variation of fundamental constants on Population III stellar evolution

Ekström

Coc

Descouvemont

et al. 2010

A&A

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“…Assuming possible changes only in the electromagnetic coupling constant, Gould et al (2006) has obtained a model dependent constraint on |Δα/α| < 2 × 10 −8 . However, when the strength of the strong interaction -the parameter Λ QCD -is also considered to be variable, the Oklo data does not provide any bound on the variation of α (Flambaum & Shuryak 2002;Chin et al 2009). …”

Section: Introductionmentioning

confidence: 99%

Searching for spatial variations ofα²/μin the Milky Way

Levshakov

Molaro²,

Reimers

2010

A&A

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Aims. We probe the dependence of α 2 /μ on the ambient matter density by means of spectral observations in submm-and mm-wave bands. Methods. A procedure is suggested for exploring the value of F = α 2 /μ, where μ = m e /m p is the electron-to-proton mass ratio, and α = e 2 /( c) is the fine-structure constant. The fundamental physical constants, which are measured in different physical environments of high (terrestrial) and low (interstellar) densities of baryonic matter are supposed to vary in chameleon-like scalar field models, which predict that both masses and coupling constant may depend on the local matter density. The parameter ΔF/F = (F obs − F lab )/F lab can be estimated from the radial velocity offset, ΔV = V rot − V fs , between the low-laying rotational transitions in carbon monoxide 13 CO and the fine-structure transitions in atomic carbon [C i]. A model-dependent constraint on Δα/α can be obtained from ΔF/F using Δμ/μ independently measured from the ammonia method. Results. Currently available radio astronomical datasets provide an upper limit on |ΔV| < 110 m s −1 (1σ). When interpreted in terms of the spatial variation of F, this gives |ΔF/F| < 3.7 × 10 −7 . An order of magnitude improvement in this limit will allow us to independently test a non-zero value of Δμ/μ = (2.2 ± 0.4 stat ± 0.3 sys ) × 10 −8 , recently found with the ammonia method. Considering that the ammonia method restricts the spatial variation of μ at the level of |Δμ/μ| ≤ 3 × 10 −8 and assuming that ΔF/F is the same in the entire interstellar medium, one obtains that the spatial variation of α does not exceed the value |Δα/α| < 2 × 10 −7 . Since extragalactic gas clouds have similar densities to those in the interstellar medium, the bound on Δα/α is also expected to be less than 2 × 10 −7 at high redshift if no significant temporal dependence of α is present.

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“…We perform the analysis on the Higgs vacuum expectation value, for three different value of κ δ D ( D ) 0 = κ δm π (m π ) 0 that is: our result (κ = −3.65), the higher limit used by Yoo & Scherrer (2003) (κ = −10) and the lower limit of the interval found by Flambaum & Shuryak (2002) (κ = 3), and considering Λ QCD fixed.…”

Section: Big Bang Nucleosynthesismentioning

confidence: 99%

“…the abundance of deuterium depends exponentially on D ). In Flambaum & Shuryak (2002; Dmitriev & Flambaum (2003); Dmitriev et al (2004); Berengut et al (2010) the variation of D as function of the quark masses was studied and the authors applied their results to set constraints using data from cosmological epochs. In Flambaum & Wiringa (2007) the dependence of nuclear binding on hadronic mass was studied.…”

Section: Introductionmentioning

confidence: 99%

Effect of the variation of the Higgs vacuum expectation value upon the deuterium binding energy and primordial abundances of D and⁴He

Mosquera

Civitarese

2010

A&A

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Aims. We calculate the constraints on the time variation of the Higgs vacuum expectation value from Big Bang Nucleosynthesis. Methods. Starting from the calculation of the deuterium binding-energy, as a function of the pion-mass and using the NN-Reid 93 potential, we calculate the abundances of primordial D and 4 He by modifying Kawano's code. The Higgs vacuum expectation value (v) and the baryon to photon ratio (η B ) enter the calculation as free parameters. By using the observational data of D and 4 He, we set constraints on η B and on the variation of v, relative to a constant value of Λ QCD . Results. Results are consistent with null variation in v and D for the early universe, within 6σ. Conclusions. We obtained a linear dependence of D upon v and found that the best-fit-value of the variation of v is null within 6σ.

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Limits on cosmological variation of strong interaction and quark masses from big bang nucleosynthesis, cosmic, laboratory and Oklo data

Cited by 85 publications

References 40 publications

Effects of the variation of fundamental constants on Population III stellar evolution

Effects of the variation of fundamental constants on Population III stellar evolution

Searching for spatial variations ofα²/μin the Milky Way

Effect of the variation of the Higgs vacuum expectation value upon the deuterium binding energy and primordial abundances of D and⁴He

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Limits on cosmological variation of strong interaction and quark masses from big bang nucleosynthesis, cosmic, laboratory and Oklo data

Cited by 85 publications

References 40 publications

Effects of the variation of fundamental constants on Population III stellar evolution

Effects of the variation of fundamental constants on Population III stellar evolution

Searching for spatial variations ofα2/μin the Milky Way

Effect of the variation of the Higgs vacuum expectation value upon the deuterium binding energy and primordial abundances of D and4He

Contact Info

Product

Resources

About

Searching for spatial variations ofα²/μin the Milky Way

Effect of the variation of the Higgs vacuum expectation value upon the deuterium binding energy and primordial abundances of D and⁴He