Baryon-Dark matter interaction in presence of magnetic fields in light of EDGES signal

Bhatt, Jitesh R.; Natwariya, Pravin Kumar; Nayak, A.; Pandey, Arun Kumar

doi:10.1140/epjc/s10052-020-7886-x

Cited by 18 publications

(12 citation statements)

References 69 publications

(82 reference statements)

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“…here, ρ γ = a r T 4 CMB , a r = 7.57 × 10 −16 J m −3 K −4 is the radiation density constant, σ T is the Thomson scattering cross-section and m e is the mass of electron. Change in the electron fraction with redshift [3,4,37,66],…”

Section: Evolution Of the Gas Temperature In The Presence Of Pmfsmentioning

confidence: 99%

“…It is to be noted that decaying MHD has been studied in several literatures. In these works, the authors consider the decay of the PMFs by ambipolar diffusion and turbulent decay [5,16,17,37,38]. Ambipolar diffusion of magnetic fields is important in neutral medium as it is inversely proportional to free-electron fraction (X e ) and X e ∼ 10 −4 after redshift z 100 [5,17,39].…”

Section: Introductionmentioning

confidence: 99%

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Constraint on primordial magnetic fields in the light of ARCADE 2 and EDGES observations

Natwariya

2021

Eur. Phys. J. C

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We study the constraints on primordial magnetic fields (PMFs) in the light of the Experiment to Detect the Global Epoch of Reionization Signature (EDGES) low-band observation and Absolute Radiometer for Cosmology, Astrophysics and Diffuse Emission (ARCADE 2). ARCADE 2 observation detected extra-galactic excess radio radiation in the frequency range 3–90 GHz. The enhancement in the radio radiation is also supported by the first station of the Long Wavelength Array (LWA1) in the frequency range 40–80 MHz. The presence of early radiation excess over the cosmic microwave background can not be completely ruled out, and it may explain the EDGES anomaly. In the presence of decaying PMFs, 21 cm differential brightness temperature can modify due to the heating of the gas by decaying magnetic fields, and we can constraint the magnetic fields. For excess radiation fraction ($$A_r$$ A r ) to be LWA1 limit, we show that the upper bound on the present-day magnetic field strength, $$B_0$$ B 0 , on the scale of 1 Mpc is $$\lesssim 3.7$$ ≲ 3.7 nG for spectral index $$n_B=-2.99$$ n B = - 2.99 . While for $$n_B=-1$$ n B = - 1 , we get $$B_0\lesssim 1.1\times 10^{-3}$$ B 0 ≲ 1.1 × 10 - 3 nG. We also discuss the effects of first stars on IGM gas evolution and the allowed value of $$B_0$$ B 0 . For $$A_r$$ A r to be LWA1 limit, we get the upper constraint on magnetic field to be $$B_0(n_B=-2.99)\lesssim 4.9\times 10^{-1}$$ B 0 ( n B = - 2.99 ) ≲ 4.9 × 10 - 1 nG and $$B_0(n_B=-1)\lesssim 3.7\times 10^{-5}$$ B 0 ( n B = - 1 ) ≲ 3.7 × 10 - 5 nG. By decreasing excess radiation fraction below the LWA1 limit, we get a more stringent bound on $$B_0$$ B 0 .

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Section: Evolution Of the Gas Temperature In The Presence Of Pmfsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Constraint on primordial magnetic fields in the light of ARCADE 2 and EDGES observations

Natwariya

2021

Eur. Phys. J. C

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“…In this respect, the Experiment to Detect the Global EoR Signature (EDGES) 5 telescope has reported an absorption profile centred at 78 MHz (Bowman et al 2018), corresponding to z ∼ 17, which has stimulated an exciting theoretical debate on its possible origin (e.g. Hektor et al 2018;Kovetz et al 2018;Bhatt et al 2020), as well as skepticism about the actual detection (Hills et al 2018). The power spectrum (PS), variance and skewness of the 21 cm signal are conceptually simple and can be used to constrain reionization (e.g.…”

Section: Introductionmentioning

confidence: 99%

Investigating X-ray sources during the epoch of reionization with the 21 cm signal

Ma,

Ciardi,

Eide

et al. 2021

Preprint

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Heating of neutral gas by energetic sources is crucial for the prediction of the 21 cm signal during the epoch of reionization (EoR). To investigate differences induced on statistics of the 21 cm signal by various source types, we use five radiative transfer simulations which have the same stellar UV emission model and varying combinations of more energetic sources, such as X-ray binaries (XRBs), accreting nuclear black holes (BHs) and hot interstellar medium emission (ISM). We find that the efficient heating from the ISM increases the average global 21 cm signal, while reducing its fluctuations and thus power spectrum. A clear impact is also observed in the bispectrum in terms of scale and timing of the transition between a positive and a negative value. The impact of XRBs is similar to that of the ISM, although it is delayed in time and reduced in intensity because of the less efficient heating. Due to the paucity of nuclear BHs, the behaviour of the 21 cm statistics in their presence is very similar to that of a case when only stars are considered, with the exception of the latest stages of reionization, when the effect of BHs is clearly visible. We find that differences between the source scenarios investigated here are larger than the instrumental noise of SKA1-low at z 7 − 8, suggesting that in the future it might be possible to constrain the spectral energy distribution of the sources contributing to the reionization process.

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“…Recently a systematical inclusion of baryon-DM interaction has been incorporated in the Boltzmann-Fokker-Planck formalism [24,25]. It ought to be noted that the baryon-DM interaction has also been considered in the literature to explain 21-cm line [26][27][28][29]. The damping of the gravitational waves in the viscous fluid can be used to constrain the mean free path and the DM mass [30,31].…”

Section: Introductionmentioning

confidence: 99%

Viscosity in cosmic fluids

2020

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The effective theory of large-scale structure formation based on $$\Lambda $$ΛCDM paradigm predicts finite dissipative effects in the resulting fluid equations. In this work, we study how viscous effect that could arise if one includes self-interaction among the dark-matter particles combines with the effective theory. It is shown that these two possible sources of dissipation can operate together in a cosmic fluid and the interplay between them can play an important role in determining dynamics of the cosmic fluid. In particular, we demonstrate that the viscosity coefficient due to self-interaction is added inversely with the viscosity calculated using effective theory of $$\Lambda $$ΛCDM model. Thus the larger viscosity has less significant contribution in the effective viscosity. Using the known bounds on $$\sigma /m$$σ/m for self-interacting darkmatter, where $$\sigma $$σ and m are the cross-section and mass of the dark-matter particles respectively, we discuss role of the effective viscosity in various cosmological scenarios.

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Baryon-Dark matter interaction in presence of magnetic fields in light of EDGES signal

Cited by 18 publications

References 69 publications

Constraint on primordial magnetic fields in the light of ARCADE 2 and EDGES observations

Constraint on primordial magnetic fields in the light of ARCADE 2 and EDGES observations

Investigating X-ray sources during the epoch of reionization with the 21 cm signal

Viscosity in cosmic fluids

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