Cross-correlation power spectra and cosmic birefringence of the CMB via photon-neutrino interaction

In the context of the standard model of particles, the weak interaction of cos-mic microwave background (CMB) and cosmic neutrino background (CvB), can generate non-vanishing TB and EB power spectra in the order of one loop forward scattering, in the presence of scalar perturbation, which is in contrast with the standard scenario cosmology. Comparing our results with the current experimental data may provide, significant infor-mation about the nature of CvB, including CMB-CvB forward scattering for TB, TE, and EB power spectra. To this end, different cases were studied, including Majorana CvB and Dirac CvB. On the other hand, it was shown that the mean opacity due to cosmic neu-trino background could behave as an anisotropic birefringent medium and change the linear polarization rotation angle. Considering the contributions from neutrino and anti-neutrino forward scattering with CMB photons (in the case of Dirac neutrino), we introduce relative neutrino and anti-neutrino density asymmetry (S & nu; = & UDelta;n & nu; n & nu; = n & nu; -n & nu; n & nu; ). Then, using the cosmic over bar birefringence angle reported by the Planck data release /3 = 0.30 & DEG; & PLUSMN; 0.11 & DEG; (68%C.L.), some constraints can be put on S & nu;. Also, the value of cosmic birefringence due to Majorana CvB medium is estimated at about /3|& nu;& SIME; 0.2 rad. In this respect, since Majorana neutrino and anti-neutrino are exactly the same, both CB contributions will be added together. However, this value is at least two orders larger than the cosmic birefringence angle reported by the Planck data release, /3 = 0.30 & DEG; & PLUSMN; 0.11 & DEG; (68%C.L.). Finally, we shortly discussed this big inconsistency. It is noteworthy that to calculate the contribution of photon-neutrino forward scattering for cosmic birefringence, we just consider the standard model of particles and the standard scenario of cosmology.