Estimating the amount of vorticity generated by cosmological perturbations in the early universe

Abstract

We estimate the amount of vorticity generated at second order in cosmological perturbation theory from the coupling between first order energy density and non-adiabatic pressure, or entropy, perturbations. Assuming power law input spectra for the source terms, and working in a radiation background, we calculate the wave number dependence of the vorticity power spectrum and its amplitude. We show that the vorticity generated by this mechanism is non-negligible on small scales, and hence should be taken into consideration in current and future CMB experiments.

arXiv comment9 pages, revtex4, 1 figure; v2: typos and minor error corrected, result unchanged

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Cited by in corpus (20)

• Calculating Non-adiabatic Pressure Perturbations during Multi-field Inflation
• The intrinsic B-mode polarisation of the Cosmic Microwave Background
• Weak lensing generated by vector perturbations and detectability of cosmic strings
• The primordial magnetic field in our cosmic backyard
• Constraint on the primordial vector mode and its magnetic field generation from seven-year Wilkinson Microwave Anisotropy Probe Observations
• Cosmic Filament Spin from Dark Matter Vortices
• Gaia: a Window to Large Scale Flows
• Effects of non-linearities on magnetic field generation
• Primordial magnetic fields generated by the non-adiabatic fluctuations at pre-recombination era
• Comparing different formulations of non-linear cosmological perturbation theory
• The magnitude of the non-adiabatic pressure in the cosmic fluid
• Cosmological Perturbations: Vorticity, Isocurvature and Magnetic Fields
• Isocurvature initial conditions for second order Boltzmann solvers
• Magnetogenesis from isocurvature initial conditions
• Recombination era magnetic fields from axion dark matter
• Effective field theory of magnetogenesis identify necessary and sufficient conditions
• The Quantum Origin of Cosmic Structure
• Double power series method for approximating cosmological perturbations
• The intrinsic bispectrum of the CMB from isocurvature initial conditions
• Non-linear effects in early Universe cosmology