Effect of primordial magnetic field on seeds for large scale structure

Yamazaki, Dai; Ichiki, Kiyotomo; Umezu, Kenichi; Hanayama, H.

doi:10.1103/physrevd.74.123518

Cited by 42 publications

(95 citation statements)

References 58 publications

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“…An explicit expression can be obtained for the ensemble averages which are used to evaluate the above spectra. In the case of a power law stochastic magnetic field we have [31,37,47,48],…”

Section: B Power Spectrum From the Pmfmentioning

confidence: 99%

“…The origin and detection of the PMF is, hence, a subject of considerable interest in modern cosmology. Moreover, the PMF could influence a variety of phenomena in the early universe [15,16,17,18] such as the cosmic microwave background (CMB) [10,19,20,21,22,23,24,25,26,27,28,29,30,31,32,33,34,35,36], and the formation of large-scale structure (LSS) [37,38,39,40,41].…”

Section: Introductionmentioning

confidence: 99%

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Constraints on the primordial magnetic field fromσ8

et al. 2008

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A primordial magnetic field (PMF) can affect the evolution of density field fluctuations in the early universe. In this paper we constrain the PMF amplitude B λ and power spectral index nB by comparing calculated density field fluctuations with observational data, i.e. the number density fluctuation of galaxies. We show that the observational constraints on cosmological density fluctuations, as parameterized by σ8, lead to strong constraints on the amplitude and spectral index of the PMF.

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“…An explicit expression can be obtained for the ensemble averages which are used to evaluate the above spectra. In the case of a power law stochastic magnetic field we have [31,37,47,48],…”

Section: B Power Spectrum From the Pmfmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Constraints on the primordial magnetic field fromσ8

et al. 2008

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“…[42][43][44] The peak position and the amplitude of the MPS is also changed by a PMF. 45,46 We can constrain the PMF parameters from the CMB and MPS observations. 47-54 When we consider the energy density of a PMF in the BBN epoch, the rate of the comic expansion is more rapid than without a PMF.…”

Section: Pmf Modelmentioning

confidence: 99%

The new hybrid BBN model with the photon cooling, X particle, and the primordial magnetic field

Yamazaki

Kusakabe

Kajino

et al. 2017

Int. J. Mod. Phys. E

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The Big Bang Nucleosynthesis theory accurately reproduces the abundances of light elements in the universes, except for the 7 Li abundance. The calculated 7 Li abundance with the baryon-to-photon ratio fixed by the observations of the cosmic microwave background (CMB) is inconsistent with the observed lithium abundances on the surface of metal-poor halo stars, and this problem is called " 7 Li problem". Previous studies proposed to resolve this 7 Li problem include photon cooling (possibly via the Bose-Einstein condensation of a scalar particle), the decay of a long-lived X particle (possibly the nextto-lightest supersymmetric particle), or an energy density of a primordial magnetic field (PMF). We review and analyze the results of these solutions both separately and in concert, and the constraint on the X particles and the PMF parameters from observed light-element abundances with a likelihood analysis. We can discover parameter ranges of the X particles which can solve the 7 Li problem and constrain the energy density of the PMF.

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“…The PMF effects on the cosmological density fields or the matter power spectrum (MPS), also, are studied by the many authors [35,52,56,[73][74][75][76][77][78][79][80][81][82]. References [73][74][75][76] groundbreaking analytical research on the effects of the first order perturbations source from PMFs on the MPS.…”

Section: Introductionmentioning

confidence: 99%

“…Then Refs. [35,52,77,78] develop the numerical method for the research on the MPS with the PMF. They make clear that these PMFs raise the MPS on the smaller scales.…”

Section: Introductionmentioning

confidence: 99%

Evolution of the cosmic matter density field with a primordial magnetic field

Yamazaki

2016

Phys. Rev. D

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A cosmological magnetic field affects the time evolution of the cosmic matter density field. The squared Alfven velocity of the cosmic fluid is proportional to an ensemble average energy density of a primordial magnetic field (PMF), and it prevents the matter density field from collapsing in the horizon scale. The matter-radiation equality time also is delayed by the presence of an ensemble average energy density of a PMF. The ensemble average energy density of the PMF also affects the matter power spectrum (MPS) through the Meszaros effect and the potential decay. Since the ensemble average energy density of the PMF is not a first order perturbation but a zero order source in the linear perturbation equations for the cosmology, to correctly understand the overall effects of the PMF on the MPS, we should significantly revise previous approaches to research for the MPS with the PMF by considering the both effects of the zero and first order sources from the PMF in the linear perturbation theory. We apply the effects of the zero order sources from the PMF to theoretical computations of the MPS for the first time. We also analyze the overall PMF effects on the MPS. The CMB polarizations are affected the weak lensing. The weak lensing is determined by the MPS. Therefore, we have to consider the zero order sources of the PMF to gain a correct understanding not only of the MPS but also the CMB polarization. * yamazaki.dai@nao.ac.jp 2

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Effect of primordial magnetic field on seeds for large scale structure

Cited by 42 publications

References 58 publications

Constraints on the primordial magnetic field fromσ8

Constraints on the primordial magnetic field fromσ8

The new hybrid BBN model with the photon cooling, X particle, and the primordial magnetic field

Evolution of the cosmic matter density field with a primordial magnetic field

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