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

被引：4

作者：

Mohammadi, Roohollah ^{[1
,2
]}

Khodagholizadeh, Jafar ^{[3
]}

Sadegh, Mahdi ^{[4
]}

Vahedi, Ali ^{[5
]}

Xue, S. S. ^{[6
,7
,8
,9
]}

机构：

[1] Iranian Natl Museum Sci & Technol INMOST, POB 11369-14611, Tehran, Iran

[2] Inst Res Fundamental Sci IPM, Sch Astron, POB 19395-5531, Tehran, Iran

[3] Farhangian Univ, POB 11876-13311, Tehran, Iran

[4] Inst Res Fundamental Sci IPM, Sch Particles & Accelerators, POB 19395-5531, Tehran, Iran

[5] Kharazmi Univ, Fac Phys, Dept Astron & High Energy Phys, POB 15614, Tehran, Iran

[6] ICRANet, Piazzale Repubbl 10, I-65122 Pescara, Italy

[7] Univ Roma La Sapienza, Phys Dept, Rome, Italy

[8] INFN, Sez Perugia, Perugia, Italy

[9] Univ Chinese Acad Sci, ICTP AP, Beijing, Peoples R China

来源：

JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS | 2023年 / 06期

关键词：

CMBR polarisation; CMBR theory; cosmological neutrinos; particle physics-cosmology connection; GRAVITY-WAVES; B-MODES; POLARIZATION; DIRAC; SIGNATURE;

D O I：

10.1088/1475-7516/2023/06/044

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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.

引用

页数：19

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