2021
DOI: 10.1093/mnras/stab2148
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Introducing SPHINX-MHD: the impact of primordial magnetic fields on the first galaxies, reionization, and the global 21-cm signal

Abstract: We present the first results from SPHINX-MHD, a suite of cosmological radiation-magnetohydrodynamics simulations designed to study the impact of primordial magnetic fields (PMFs) on galaxy formation and the evolution of the intergalactic medium (IGM) during the epoch of reionization. The simulations are among the first to employ multi-frequency, on-the-fly radiation transfer and constrained transport ideal MHD in a cosmological context to simultaneously model the inhomogeneous process of reionization as well a… Show more

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Cited by 46 publications
(22 citation statements)
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References 228 publications
(300 reference statements)
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“…The second type is a tangled magnetic field that follows a magnetic energy spectrum with spectral index 𝑛 𝐵 . The tangled magnetic initial conditions (ICs; Martin-Alvarez et al in prep.; but also similar to those employed in Katz et al 2021) are produced by modulating the spectrum of the vector potential at each Fourier wavelength 𝑘 and requiring the magnetic energy spectra produced by its curl to have a spectral slope 𝑛 𝐵 . All our magnetic ICs assume 𝑛 𝐵 = 3/2 to reproduce a Kazantsev spectrum (Kazantsev 1968) corresponding to the magnetic inversecascade characteristic of a tangled ISM (Bhat & Subramanian 2013; 1 https://bitbucket.org/rteyssie/ramses/src/master/ Martin-Alvarez et al 2018).…”
Section: Numerical Methods and Initial Conditionsmentioning
confidence: 99%
“…The second type is a tangled magnetic field that follows a magnetic energy spectrum with spectral index 𝑛 𝐵 . The tangled magnetic initial conditions (ICs; Martin-Alvarez et al in prep.; but also similar to those employed in Katz et al 2021) are produced by modulating the spectrum of the vector potential at each Fourier wavelength 𝑘 and requiring the magnetic energy spectra produced by its curl to have a spectral slope 𝑛 𝐵 . All our magnetic ICs assume 𝑛 𝐵 = 3/2 to reproduce a Kazantsev spectrum (Kazantsev 1968) corresponding to the magnetic inversecascade characteristic of a tangled ISM (Bhat & Subramanian 2013; 1 https://bitbucket.org/rteyssie/ramses/src/master/ Martin-Alvarez et al 2018).…”
Section: Numerical Methods and Initial Conditionsmentioning
confidence: 99%
“…The UHECR bound on large correlation length cosmological magnetic field (that would originate from Inflation) is stronger than the limit from non-observation of magnetic field induced excess optical depth of CMB signal [29] and is somewhat weaker than the limit imposed by non-observation of faster recombination [30]. Closeness of the bounds from three different techniques indicates that improvement of the sensitivity of these techniques may result in a "multi-messenger" detection of inflationary cosmological magnetic field, if it has scale-invariant power spectrum and the field strength close to B ∼ 10 −10 G.…”
mentioning
confidence: 86%
“…The bound from Faraday rotation is from [28]. The "CMB scattering" bound is from [29]. The "CMB clumping" bound is from [30].…”
mentioning
confidence: 99%
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“…Current observational constraints cannot rule out strong PMFs, but provide a conservative comoving magnetic field strength upper limit of 𝐵 0 < 10 −9 G, obtained by Planck Collaboration (2015) 1 . Numerical studies offer a promising avenue to further understand the origin and evolution of galactic magnetic fields, for example, by studying the evolution of magnetic fields with different origins (Martin-Alvarez et al 2021;Garaldi et al 2021) and predicting observables upon which strong PMFs may have an impact on, such as galactic properties (Martin-Alvarez et al 2020), supermassive black hole masses (Pillepich et al 2018), the population of galaxies or cosmic reionization (Sanati et al 2020;Katz et al 2021).…”
Section: Introductionmentioning
confidence: 99%