Influence of electron-positron pairs on the wakefields in plasmas

Berezhiani, V. I.; Tsintsadze, Levan N.; Shukła, P. K.

doi:10.1088/0031-8949/46/1/010

Cited by 46 publications

(26 citation statements)

References 5 publications

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“…where the coupling strength is, in turn, proportional to the axion mass m a [4,14,15]. Figure 1 shows the relation between m a and n a computed for the thermalisation processes (1.1) based on the original calculations of reference [4].…”

Section: Introductionmentioning

confidence: 99%

Neutrino and axion hot dark matter bounds after WMAP-7

Hannestad

Mirizzi

Raffelt

et al. 2010

J. Cosmol. Astropart. Phys.

101

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Abstract. We update cosmological hot dark matter constraints on neutrinos and hadronic axions. Our most restrictive limits use 7-year data from the Wilkinson Microwave Anisotropy Probe for the cosmic microwave background anisotropies, the halo power spectrum (HPS) from the 7th data release of the Sloan Digital Sky Survey, and the Hubble constant from Hubble Space Telescope observations. We find 95% CL upper limits of m ν < 0.44 eV (no axions), m a < 0.91 eV (assuming m ν = 0), and m ν < 0.41 eV and m a < 0.72 eV for two hot dark matter components after marginalising over the respective other mass. CMB data alone yield m ν < 1.19 eV (no axions), while for axions the HPS is crucial for deriving m a constraints. This difference can be traced to the fact that for a given hot dark matter fraction axions are much more massive than neutrinos.Neutrino and axion hot dark matter bounds after WMAP-7 2

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Section: Introductionmentioning

confidence: 99%

Neutrino and axion hot dark matter bounds after WMAP-7

Hannestad

Mirizzi

Raffelt

et al. 2010

J. Cosmol. Astropart. Phys.

101

View full text Add to dashboard Cite

show abstract

“…The presence of the hypercharge for Q allows for their mixing with the SM quarks, making it possible for them to decay, avoiding the problem of their overabundance [31,32]. Furthermore, one needs an additional U (1) P Q symmetry which acts as a chiral rotation on Q and as a phase rotation of X .…”

Section: The Simplest Modelmentioning

confidence: 99%

A minimal scale invariant axion solution to the strong CP-problem

Tokareva

2018

Eur. Phys. J. C

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We present a scale-invariant extension of the Standard model allowing for the Kim-Shifman-VainsteinZakharov (KSVZ) axion solution of the strong CP problem in QCD. We add the minimal number of new particles and show that the Peccei-Quinn scalar might be identified with the complex dilaton field. Scale invariance, together with the Peccei-Quinn symmetry, is broken spontaneously near the Planck scale before inflation, which is driven by the Standard Model Higgs field. We present a set of general conditions which makes this scenario viable and an explicit example of an effective theory possessing spontaneous breaking of scale invariance. We show that this description works both for inflation and low-energy physics in the electroweak vacuum. This scenario can provide a self-consistent inflationary stage and, at the same time, successfully avoid the cosmological bounds on the axion. Our general predictions are the existence of colored TeV mass fermion and the QCD axion. The latter has all the properties of the KSVZ axion but does not contribute to dark matter. This axion can be searched via its mixing to a photon in an external magnetic field.

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“…Based on the above arguments, we assume the possibility that the Bose-Einstein condensation might have happened during the early stages of cosmological evolution of the universe with a temperature comparable to the critical temperature for Bose-Einstein condensation T cr ∼ 2πh 2 n 2/3 /mk B where m is the particle mass, n is the particle density, and k B is Boltzmann's constant [17][18][19][20][21][22][23][24][25][26][27][28][29][30][31][32].…”

Section: Introductionmentioning

confidence: 99%

Dark matter as the Bose–Einstein condensation in loop quantum cosmology

Atazadeh¹,

Darabi²,

Mousavi³

2016

Eur. Phys. J. C

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We consider the FLRW universe in a loop quantum cosmological model filled with radiation, baryonic matter (with negligible pressure), dark energy, and dark matter. The dark matter sector is supposed to be of Bose-Einstein condensate type. The Bose-Einstein condensation process in a cosmological context by supposing it as an approximate first-order phase transition, has already been studied in the literature. Here, we study the evolution of the physical quantities related to the early universe description such as the energy density, temperature, and scale factor of the universe, before, during, and after the condensation process. We also consider in detail the evolution era of the universe in a mixed normal-condensate dark matter phase. The behavior and time evolution of the condensate dark matter fraction is also analyzed.

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Influence of electron-positron pairs on the wakefields in plasmas

Cited by 46 publications

References 5 publications

Neutrino and axion hot dark matter bounds after WMAP-7

Neutrino and axion hot dark matter bounds after WMAP-7

A minimal scale invariant axion solution to the strong CP-problem

Dark matter as the Bose–Einstein condensation in loop quantum cosmology

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