PRIMORDIAL MAGNETIC FIELDS WITH BPOL

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MAGNETIC PERTURBATIONS  SIMPLEST MODEL OF PMF SUPPORTED IN FRW IS A STOCHASTIC  BACKGROUND OF PMF WITH POWER LAW POWER SPECTRA  PMF GENERATES SCALAR VECTOR AND TENSOR MODES.  MAGNETIC SCALAR MODE IS  SOURCED BY MAGNETIC  ENERGY DENSITY AND  SCALAR ANISOTROPIC  STRESS  PMF INDUCE A LORENTZ FORCE  ON BARYONS WHICH AFFECTS  BOTH SCALAR AND VECTOR  PERTURBATIONS  MAGNETIC VECTOR AND TENSOR  MODES ARE SOURCED BY  MAGNETIC VECTOR AND TENSOR  ANISOTROPIC STRESSES  THE DOMINANT CONTRIBUTIONS TO CMB ANISOTROPIES IS  REPRESENTED BY SCALAR PERTURBATIONS ON LARGE SCALES  AND BY VECTOR PERTURBATIONS ON SMALL SCALES.  THE TENSOR CONTRIBUTION REMAINS SUBDOMINANT  4 4 
NOTE HOW THE DOMINANT CONTRIBUTION IS THE VECTOR ONE  AND THAT THE TENSOR MODE ALWAYS REMAINS SUBDOMINANT  WITH RESPECT TO THE OTHER TWO.  5 5 
Page 1 and 2: PRIMORDIAL MAGNETIC FIELDS  W
Page 3: REFERENCES  Finelli, Paci &
Page 7 and 8: PMF AND BPOL I  Solid: Ad
Page 9 and 10: COSMOLOGICAL PARAMETERS AND P
Page 11 and 12: MAGNETIC NON GAUSSIANITIES

PRIMORDIAL MAGNETIC FIELDS WITH BPOL

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