Photon-neutrino scattering and the<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>B</mml:mi></mml:math>-mode spectrum of CMB photons

Khodagholizadeh, Jafar; Mohammadi, Rohoollah; Xue, She‐Sheng

doi:10.1103/physrevd.90.091301

Cited by 15 publications

(17 citation statements)

References 40 publications

(45 reference statements)

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“…Therefore, similar to CMB, it contains very helpful information about early universe. Here we use the time evolution of GRB polarization due to photon-neutrino interactions [15,21] …”

Section: Grbs and Cosmic Neutrino Background Forward Scatteringmentioning

confidence: 99%

Generation of circular polarization of gamma ray bursts

Batebi

Mohammadi²,

Ruffini

et al. 2016

Phys. Rev. D

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The generation of the circular polarization of Gamma Ray Burst (GRB) photons is discussed in this paper via their interactions with astro-particles in the presence or absence of background fields such as magnetic fields and non-commutative space time geometry. Solving quantum Boltzmann equation for GRB-photons as a photon ensemble, we discuss the generation of circular polarization (as Faraday conversion phase shift ∆φ F C ) of GRBs in the following cases: (i) intermediate interactions, i.e. the Compton scattering of GRBs in the galaxy cluster magnetic field and in the presence of non-commutative space time geometry, as well as the scattering of GRBs in cosmic neutrino background (CNB), and in cosmic microwave background (CMB); (ii) interactions with particles and fields in shock wave, i.e. the Compton scattering of GRBs with accelerated charged particles in the presence of magnetic fields. We found that (i) after shock wave crossing, the most contribution of ∆φ F C for energetic GRBs (in order GeV and larger) comes from GRB-CMB interactions, however for low energy GRBs the contributions of the Compton scattering of GRBs in the galaxy cluster magnetic field dominate; (ii) in shock wave crossing, the magnetic filed has significant effects on converting GRB's linear polarization to circular one, this effect can be used to better understanding magnetic profile in shock wave. The main aim of this work is a emphasis that the studying and measuring the circular polarization of GRBs are helpful for better understanding of physics and mechanism of the generation of GRBs and their interactions before reaching us.

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“…Therefore, similar to CMB, it contains very helpful information about early universe. Here we use the time evolution of GRB polarization due to photon-neutrino interactions [15,21] …”

Section: Grbs and Cosmic Neutrino Background Forward Scatteringmentioning

confidence: 99%

Generation of circular polarization of gamma ray bursts

Batebi

Mohammadi²,

Ruffini

et al. 2016

Phys. Rev. D

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“…The BICEP2 data could be explained by the scalar and tensor modes from primordial magnetic fields [2]. The interaction between CMB photons and CNB Neutrinos can produce the B-mode spectrum [5] even with the scalar perturbation only. The Planck group presented discussions that the result of BICEP2 can be fully attributed to cosmic dust [6].…”

Section: Introductionmentioning

confidence: 98%

B-mode polarization of the CMB and the cosmic neutrino background

Mohammadi¹,

Khodagholizadeh

Sadegh

et al. 2016

Phys. Rev. D

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It is known that in contrast with the E-mode polarization, the B-mode polarization of the Cosmic Microwave Background cannot be generated by the Compton scattering in the case of scalar mode of metric perturbation. However it is possible to generate the B-mode by the Compton scattering in the case of tensor mode of metric perturbation. For this reason, the ratio of tensor to scalar modes of metric perturbation (r ∼ C Bl /C El ) is estimated by comparing the B-mode power spectrum with the E-mode at least for small l. We study the CMB polarization specially B-mode due to the weak interaction of Cosmic Neutrino Background (CNB) and CMB, in addition to the Compton scattering in both cases of scalar and tensor metric perturbations. It is shown that the power spectrum C Bl of the B-mode polarization receives some contributions from scalar and tensor modes, which have effects on the value of r-parameter. We also show that the B-mode polarization power spectrum can be used as an indirect probe into the CNB.

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“…The B-mode not only helps to estimate r-parameter but also it can be used to constrain the bound on the strength of primordial magnetic field [30], the neutrino masses [31], modification of the gravity [32,33], cosmic (super-) string [34][35][36] and other fundamental physics [37]. Also in recent years, many mechanisms have been reported which are capable to generate the magnetic like polarization [38][39][40][41][42][43][44][45][46][47][48][49]. Also it is worthwhile to note, the small field models of inflation can generate a significant primordial gravitational wave signal which predicts a value of r parameter as high as 0.01 [50].…”

Section: Introductionmentioning

confidence: 99%

“…Some of our recent works also discussed the generation of B-mode polarization in the presence of scalar perturbations via Cosmic Neutrino Background and CMB interactions [47,59,60], nonlinear photons interactions [61], photon interaction by considering extensions to QED such as Lorentzinvariant violating operators [62], non-commutative geometry [49], interaction of dipolar dark matter with CMB photons [63] and photon-fermion forward scattering [64]. Also the intrinsic B-mode polarization is calculated by using the Boltzmann code SONG [65] which induce in the CMB by the evolution of primordial density perturbations at second order [66].…”

Section: Introductionmentioning

confidence: 99%

B-mode power spectrum of CMB via polarized Compton scattering

Khodagholizadeh

Mohammadi

Sadegh

et al. 2020

J. Cosmol. Astropart. Phys.

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In this work, according to some evidence from being an asymmetry in the number density of left and right-handed electrons, δ L , in-universe motivate us to calculate the dominated contribution of this asymmetry in the generation of B-mode power spectrum C (S) B l . Note, in the standard cosmological scenario, Compton scattering in the presence of scalar matter perturbation can not generate magnetic like pattern in linear polarization while in the case of polarized Compton scattering, we have shown C (S) B l ∝ δ 2 L . We add up the spectrum of the B-mode generated by the polarized Compton scattering to the spectra produced by weak lensing effects and Compton scattering in the presence of tensor perturbations. The resultsshow a significant amplification in C B l in large scale l < 500 for δ L > 10 −6 which will be observable in future high resolution B-mode polarization detection. Finally, we have shown that C (S) B l generated by polarized Compton scattering can suppress the tensor to scalar ratio, r parameter so that this contamination can be comparable to a primordial tensor-to-scalar ratio spatially for δ L > 10 −5 . PACS numbers: 13.15.+g, 98.80.Es, 98.70.Vc. a j.gholizadeh@cgu.ac.ir b rmohammadi@ipm.ir c m.sadegh@pnu.ac.ir d vahedi@khu.ac.ir,vahedi@ipm.ir2

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Photon-neutrino scattering and theB-mode spectrum of CMB photons

Cited by 15 publications

References 40 publications

Generation of circular polarization of gamma ray bursts

Generation of circular polarization of gamma ray bursts

B-mode polarization of the CMB and the cosmic neutrino background

B-mode power spectrum of CMB via polarized Compton scattering

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