CMB anisotropies from primordial inhomogeneous magnetic fields

By A. Lewis. 2004

151 citations recorded by the source corpus.

Primordial inhomogeneous magnetic fields of the right strength can leave a signature on the CMB temperature anisotropy and polarization. Potentially observable contributions to polarization B-modes are generated by vorticity and gravitational waves sourced by the magnetic anisotropic stress. We compute the corresponding CMB transfer functions in detail including the effect of neutrinos. The shear rapidly causes the neutrino anisotropic stress to cancel the stress from the magnetic field, suppressing the production of gravitational waves and vorticity on super-horizon scales after neutrino decoupling. A significant large scale signal from tensor modes can only be produced before neutrino decoupling, and the actual amplitude is somewhat uncertain. Plausible values suggest primordial nearly scale invariant fields of ~ 10^(-10)G today may be observable from their large scale tensor anisotropy. They can be distinguished from primordial gravitational waves by their non-Gaussianity. Vector mode vorticity sources B-mode power on much smaller scales with a power spectrum somewhat similar to that expected from weak lensing, suggesting amplitudes ~ 10^(-9)G may be observable on small scales for a spectral index of n ~ -2.9. In the appendix we review the covariant equations for computing the vector and tensor CMB power spectra that we implement numerically.

Subfields: Astronomy and Astrophysics, Oceanography

View Paper: https://www.semanticscholar.org/paper/3118e1cdf00eedef99de4a9a6c0301c3df28f7ab

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In Astronomy and Astrophysics

1. Andrii Y. Neronov
2. R. Durrer
3. C. Caprini
4. G. Servant
5. L. Sorbo
6. Jean-Philippe Uzan
7. P. Hintz
8. András Vasy

In Oceanography

1. Andrii Y. Neronov
2. R. Durrer

Citations in the corpus

• Planck 2015 results: XIX. Constraints on primordial magnetic fields (2015, unknown): “We use the initial conditions derived by Lewis (2004), Paoletti et al. (2009), Paoletti & Finelli (2011), and Shaw & Lewis (2010) for scalar and compensated tensor modes, vector modes, and passive modes, respectively.”
• Cosmological Magnetic Fields: Their Generation, Evolution and Observation (2013, methodology): “Magnetic fields lead to strong vector perturbations which generate significant B-polarization (Seshadri and Subramanian 2001; Lewis 2004).”