Inflationary Affleck-Dine scalar dynamics and isocurvature perturbations

Enqvist, Kari; McDonald, John

doi:10.1103/physrevd.62.043502

Cited by 50 publications

(61 citation statements)

References 44 publications

(37 reference statements)

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“…Residual isocurvature fluctuations can be generated when there exist multiple components with different origins, which are associated with dark matter, baryon and neutrino [2] #1 . Such examples include axion [5,6,7,8,9,10,11,12] and AffleckDine baryogenesis [13,14,15], where cold dark matter (CDM) and baryon isocurvature modes can be respectively generated. These isocurvature modes are basically uncorrelated with adiabatic ones, however, when one considers a scenario where a light scalar field other than the inflaton is responsible for (adiabatic) density fluctuation such as the curvaton model [16,17,18], isocurvature perturbations can be correlated with the adiabatic ones and be easily generated, depending on how and when CDM and baryon are created [19,20,21,22,23,24,25,26,27,28,29,30,31].…”

Section: Introductionmentioning

confidence: 99%

CMB constraint on non-Gaussianity in isocurvature perturbations

Hikage

Kawasaki

Sekiguchi

et al. 2013

J. Cosmol. Astropart. Phys.

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We study the CMB constraints on non-Gaussianity in CDM isocurvature perturbations. Non-Gaussian isocurvature perturbations can be produced in various models at the very early stage of the Universe. Since the isocurvature perturbations little affect the structure formation at late times, CMB is the best probe of isocurvature non-Gaussianity at least in the near future. In this paper, we focus on non-Gaussian curvature and isocurvature perturbations of the local-type, which are uncorrelated and in the form, and constrain the non-linearity parameter of isocurvature perturbations, f (ISO) NL , as well as the curvature one f NL . For this purpose, we employ several state-of-art techniques for the analysis of CMB data and simulation. Assuming that isocurvature perturbations are subdominant, we apply our method to the WMAP 7-year data of temperature anisotropy and obtain constraints on a combination α 2 f (ISO) NL , where α is the ratio of the power spectrum of isocurvature perturbations to that of the adiabatic ones. When the adiabatic perturbations are assumed to be Gaussian, we obtained a constraint α 2 f (ISO) NL = 40 ± 66 assuming the power spectrum of isocurvature perturbations is scale-invariant. When we assume that the adiabatic perturbations can also be non-Gaussian, we obtain f NL = 38 ± 24 and α 2 f (ISO) NL = −8 ± 72. We also discuss implications of our results for the axion CDM isocurvature model.

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Section: Introductionmentioning

confidence: 99%

CMB constraint on non-Gaussianity in isocurvature perturbations

Hikage

Kawasaki

Sekiguchi

et al. 2013

J. Cosmol. Astropart. Phys.

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“…This is because isocurvature fluctuations might be produced depending on how dark matter/baryon number is generated. Such examples are axion [2][3][4][5][6][7][8] and AffleckDine baryogenesis mechanism [9][10][11][12] in which CDM and baryon isocurvature fluctuations can respectively be generated #1 . If such a mode is found to be non-zero, it would give invaluable information on CDM/baryogenesis scenarios.…”

Section: Introductionmentioning

confidence: 99%

Differentiating CDM and baryon isocurvature models with 21 cm fluctuations

Kawasaki

Sekiguchi

Takahashi

2011

J. Cosmol. Astropart. Phys.

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We discuss how one can discriminate models with cold dark matter (CDM) and baryon isocurvature fluctuations. Although current observations such as cosmic microwave background (CMB) can severely constrain the fraction of such isocurvature modes in the total density fluctuations, CMB cannot differentiate CDM and baryon ones by the shapes of their power spectra. However, the evolution of CDM and baryon density fluctuations are different for each model, thus it would be possible to discriminate those isocurvature modes by extracting information on the fluctuations of CDM/baryon itself. We discuss that observations of 21 cm fluctuations can in principle differentiate these modes and demonstrate to what extent we can distinguish them with future 21 cm surveys. We show that, when the isocurvature mode has a large blue-tilted initial spectrum, 21 cm surveys can clearly probe the difference.

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“…[33], where this model has been embedded in a supersymmetric theory in four dimensions. Like in the case of AD baryogenesis [31], our setup can be tested by the forthcoming accurate measurements of the spectral index of the microwave background; our model predicts a very flat spectrum.…”

Section: B Dynamics Of Ad Fieldmentioning

confidence: 99%

“…In the regime when the main inflationary potential is due to the inflaton sector, the slow-roll parameter |η| can be written as [31] …”

Section: The Modelmentioning

confidence: 99%

Baryogenesis in theories with large extra spatial dimensions

Allahverdi¹,

Enqvist²,

Mazumdar³

et al. 2001

Nuclear Physics B

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We describe a simple and predictive scenario for baryogenesis in theories with large extra dimensions which resembles Affleck-Dine baryogenesis. The Affleck-Dine field is a complex scalar field carrying a U (1) χ charge which is dynamically broken after the end of inflation. This generates an excess of χ overχ, which then decays into Standard Model fermions to produce an excess of baryons over anti-baryons. Our model is very constrained because the Affleck-Dine field has to be sufficiently flat during inflation. It is also a source for density fluctuations which can be tested in the coming satellite and balloon experiments.

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Inflationary Affleck-Dine scalar dynamics and isocurvature perturbations

Cited by 50 publications

References 44 publications

CMB constraint on non-Gaussianity in isocurvature perturbations

CMB constraint on non-Gaussianity in isocurvature perturbations

Differentiating CDM and baryon isocurvature models with 21 cm fluctuations

Baryogenesis in theories with large extra spatial dimensions

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