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http://eprints.org/relation/isVersionOf http://eprints.iliauni.edu.ge/id/document/2823 http://eprints.org/relation/isVolatileVersionOf http://eprints.iliauni.edu.ge/id/document/2823 http://eprints.org/relation/ismediumThumbnailVersionOf http://eprints.iliauni.edu.ge/id/document/2823 2834 2 8093 document 2834 small.jpg image/png 6b834ffe00be0f974ce27493579b4759 MD5 1742 2014-01-27 20:49:06 http://eprints.iliauni.edu.ge/730/6/small.jpg 730 6 6 image/png other Thumbnails conversion from text to thumbnail_small ge public

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http://eprints.org/relation/isVersionOf http://eprints.iliauni.edu.ge/id/document/2823 http://eprints.org/relation/isVolatileVersionOf http://eprints.iliauni.edu.ge/id/document/2823 http://eprints.org/relation/issmallThumbnailVersionOf http://eprints.iliauni.edu.ge/id/document/2823 archive 131 disk0/00/00/07/30 2014-01-30 12:33:36 2015-03-27 06:52:44 2014-01-30 12:33:36 article show Durrer Ruth Ferreira Pedro Kahniashvili Tina tinatin@iliauni.edu.ge pub QC public We derive an expression for the angular power spectrum of cosmic microwave background anisotropies due to gravity waves generated by a stochastic magnetic field and compare the result with current observations; we take into account the non-linear nature of the stress energy tensor of the magnetic field. For almost scale invariant spectra, the amplitude of the magnetic field at galactic scales is constrained to be of order 10-9 G. If we assume that the magnetic field is damped below the Alfvén damping scale, we find that its amplitude at 0.1h-1 Mpc, Bλ, is constrained to be Bλ<7.9×10-6e3n G, for n<-3/2, and Bλ<9.5×10-8e0.37n G, for n>-3/2, where n is the spectral index of the magnetic field and H0=100h km s-1 Mpc-1 is the Hubble constant today. 2000 published Physical review D 61 043001 TRUE