Generation of the CMB cosmic birefringence through axion-like particles, sterile and active neutrinos

The cosmic birefringence (CB) angle refers to the rotation of the linear polarization plane of Cosmic Microwave Background (CMB) radiations when parity-violating theories are considered. We analyzed the Quantum Boltzmann equation for an ensemble of CMB photons interacting with the right-handed steri...

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Bibliographic Details
Published in:The European physical journal. C, Particles and fields Particles and fields, 2024-06, Vol.84 (6), p.619-13, Article 619
Main Authors: Mahmoudi, Somayyeh, Sadegh, Mahdi, Khodagholizadeh, Jafar, Motie, Iman, Xue, She-Sheng, Blanchard, Alain
Format: Article
Language:English
Subjects:
Astronomy
Astrophysics and Cosmology
Birefringence
Boltzmann transport equation
Cosmic microwave background
Dark matter
Elementary Particles
Hadrons
Heavy Ions
Hypothetical particles
Linear polarization
Measurement Science and Instrumentation
Neutrinos
Nuclear Energy
Nuclear Physics
Physics
Physics and Astronomy
Quantum Field Theories
Quantum Field Theory
Regular Article - Theoretical Physics
String Theory
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Summary:The cosmic birefringence (CB) angle refers to the rotation of the linear polarization plane of Cosmic Microwave Background (CMB) radiations when parity-violating theories are considered. We analyzed the Quantum Boltzmann equation for an ensemble of CMB photons interacting with the right-handed sterile neutrino dark matter (DM) and axion-like particles (ALPs) DM in the presence of the scalar metric perturbation. We used the birefringence angle of CMB to study those probable candidates of DM. It is shown that the CB angle contribution of sterile neutrino is much less that two other sources considered here. Next, we combined the results of the cosmic neutrinos’ contribution and the contribution of the ALPs to producing the CMB birefringence and discussed the uncertainty on the parameter space of axions caused by the share of CMB-cosmic neutrino interaction in generating this effect. Finally, we plotted the EB power spectrum of the CMB and showed that this spectrum behaves differently in the presence of cosmic neutrinos and ALPs interactions in small l . Hence, future observed data for C EB l , will help us to distinguish the CB angle value due to the various sources of its production.
ISSN:1434-6052
1434-6044
1434-6052
DOI:10.1140/epjc/s10052-024-13004-0