Observational Implications of Axionic Isocurvature Fluctuations

Kanazawa, Takeshi; Kawasaki, Masahiro; Sugiyama, Naoshi; Yanagida, Tsutomu T.

doi:10.1143/ptp.102.71

Cited by 12 publications

(6 citation statements)

References 30 publications

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“…It is sometimes useful to consider the ratio α of the total power spectra, defined as P tot = P ad + P iso [208,204], where α is defined as [204] α = 16 25…”

Section: Isocurvature Perturbations and Cmbmentioning

confidence: 99%

“…where δθ ≈ (H/2πφ) is generated by quantum fluctuations of the AD field at the time when the perturbations cross the horizon. The magnitude of the CMB isocurvature perturbation relative to the adiabatic perturbation can be written as [53,203,208],…”

Section: Isocurvature Fluctuations In D-term Inflationmentioning

confidence: 99%

“…Present CMB and large-scale structure observations require that α < ∼ 0.1 [203,208]. COBE normalization combined with the value of σ 8 (the rms of the density field on a scale of 8 Mpc) as obtained from X-ray observations of the local cluster together with the shape parameter Γ ≈ Ω m h = 0.25 ± 0.05 [333] from galaxy surveys, which is also consistent with the recent observations of high-redshift supernovae [20,21]) yields the limit α < ∼ 0.07.…”

Section: Isocurvature Fluctuations In D-term Inflationmentioning

confidence: 99%

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Cosmological consequences of MSSM flat directions

2003

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We review the cosmological implications of the flat directions of the Minimally Supersymmetric Standard Model (MSSM). We describe how field condensates are created along the flat directions because of inflationary fluctuations.The post-inflationary dynamical evolution of the field condensate can charge up the condensate with B or L in a process known as Affleck-Dine baryogenesis. Condensate fluctuations can give rise to both adiabatic and isocurvature density perturbations and could be observable in future cosmic microwave experiments. In many cases the condensate is however not the state of lowest energy but fragments, with many interesting cosmological consequences. Fragmentation is triggered by inflation-induced perturbations and the condensate lumps will eventually form non-topological solitons, known as Q-balls. Their proper-1 ties depend on how supersymmetry breaking is transmitted to the MSSM; if by gravity, then the Q-balls are semi-stable but long-lived and can be the source of all the baryons and LSP dark matter; if by gauge interactions, the Q-balls can be absolutely stable and form dark matter that can be searched for directly.We also discuss some cosmological applications of generic flat directions and Qballs in the context of self-interacting dark matter, inflatonic solitons and extra dimensions.1 kari.enqvist@helsinki.fi 2 a

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“…It is sometimes useful to consider the ratio α of the total power spectra, defined as P tot = P ad + P iso [208,204], where α is defined as [204] α = 16 25…”

Section: Isocurvature Perturbations and Cmbmentioning

confidence: 99%

Section: Isocurvature Fluctuations In D-term Inflationmentioning

confidence: 99%

Section: Isocurvature Fluctuations In D-term Inflationmentioning

confidence: 99%

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Cosmological consequences of MSSM flat directions

2003

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“…It is also useful to consider the ratio α of the present power spectra [13]. The present power spectrum can be described as…”

Section: Isocurvature Fluctuationsmentioning

confidence: 99%

Adiabatic and isocurvature fluctuations of Affleck–Dine field in D-term inflation model

Kawasaki

Takahashi

2001

Physics Letters B

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We reconsider fluctuations of Affleck-Dine (AD) field in a D-term inflation model. Contrary to the previous analysis, we find that the spectrum of the adiabatic fluctuations is almost scale invariant even if the AD field has a large initial value. Furthermore, we study the isocurvature fluctuations of the AD field and estimate the ratio of the isocurvature to adiabatic power spectrum. The dynamics of the inflaton and AD fields sets the upper bound for the value of the AD field, leading to a lower limit for isocurvature perturbation. It is shown that the recent Cosmic Microwave Background data give a constraint on the D-term inflation and the AD field.

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“…However, isocurvature perturbations have been shown to be of potential importance in some specific models : axions [4], [5], [7], [12], Affleck-Dine baryogenesis mechanism [13], multiple field inflation [10], [11], [14], [15].…”

Section: Introductionmentioning

confidence: 99%

Correlated mixtures of adiabatic and isocurvature cosmological perturbations

Langlois

Riazuelo

2000

Phys. Rev. D

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We examine the consequences of the existence of correlated mixtures of adiabatic and isocurvature perturbations on the CMB and large scale structure. In particular, we consider the four types of "elementary" totally correlated hybrid initial conditions, where only one of the four matter species (photons, baryons, neutrinos, CDM) deviates from adiabaticity. We then study the height and position of the acoustic peaks with respect to the large angular scale plateau as a function of the isocurvature to adiabatic ratio.

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Observational Implications of Axionic Isocurvature Fluctuations

Cited by 12 publications

References 30 publications

Cosmological consequences of MSSM flat directions

Cosmological consequences of MSSM flat directions

Adiabatic and isocurvature fluctuations of Affleck–Dine field in D-term inflation model

Correlated mixtures of adiabatic and isocurvature cosmological perturbations

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