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scale given by [ref] k_J=[14.8(Ω_m0.3)^0.5(h0.7)(B_01 nG)^-1]^2/n__B+5 Mpc^-1 , which appears as a hard cut-off to the magnetically induced matter power spectrum in our calculations.","intent_p":0.9,"contests_p":null},{"arxiv_id":"2312.11448","title":"Cosmic Recombination in the Presence of Primordial Magnetic Fields","url":"/paper/2312.11448","section":"The combined effects of plasma heating and baryon clumping","sentence":"These authors used an analytic expression from [ref] to approximate the heating rate due to magnetic field dissipation.","intent_p":0.95,"contests_p":null}]},{"kind":"data_used","label":"Uses its data or values","papers":1,"sentences":1,"quotes":[{"arxiv_id":"2402.18565","title":"Primordial Magnetic Fields in Light of Dark Ages Global 21-cm Signal","url":"/paper/2402.18565","section":"Primordial magnetic fields","sentence":"Here, $γ_e$ is the ion-neutral coupling coefficient, which can be approximated as $γ_e ≈1.9×10^14(T_g/K)^0.375cm^3/g/s$ [ref] 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sufficiently large $σ_B,0$ and blue spectral indices ($n_B ≳-2.9$), PMFs can dominate $σ(M,z)$ at low masses, substantially boosting early halo formation [ref] .","intent_p":0.97,"contests_p":null}]},{"kind":"background","label":"Cites it as background","papers":15,"sentences":19,"quotes":[{"arxiv_id":"2010.08836","title":"Imprints of the post recombination dissipation of helical magnetic field on the Cosmic Microwave Background Radiation","url":"/paper/2010.08836","section":"Introduction","sentence":"In the standard model of post-recombination universe, the temperature of the IGM follows the CMB temperature up to a redshift of $z ≈100$ after which it thermally decouples from CMB and evolves as $a^-2$ at low redshifts [ref] .","intent_p":0.98,"contests_p":null},{"arxiv_id":"2312.11448","title":"Cosmic Recombination in the Presence of Primordial Magnetic Fields","url":"/paper/2312.11448","section":"The combined effects of plasma heating and baryon clumping","sentence":"It is well known [ref] that the decay of magnetic turbulence induces a heat source for the baryons which may influence the ionization fraction $X_e$ substantially at lower redhifts.","intent_p":0.9,"contests_p":null},{"arxiv_id":"2402.18565","title":"Primordial Magnetic Fields in Light of Dark Ages Global 21-cm Signal","url":"/paper/2402.18565","section":"Primordial magnetic fields","sentence":"Ambipolar diffusion is important when plasma is partially ionized, whereas non-linear effects can lead to turbulent decay [ref] .","intent_p":0.88,"contests_p":null},{"arxiv_id":"2411.03183","title":"Revisiting constraints on primordial magnetic fields from spectral distortions of cosmic microwave background","url":"/paper/2411.03183","section":"Introduction","sentence":"In this paper, we focus specifically on how the spectral distortions [ref] of the cosmic microwave background (CMB) can impose constraints on the properties of primordial magnetic fields [ref] 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