2012
DOI: 10.1016/j.physletb.2012.10.067
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Gravitational instability of the primordial plasma: Anisotropic evolution of structure seeds

Abstract: We study how the presence of a background magnetic field, of intensity compatible with current observation constraints, affects the linear evolution of cosmological density perturbations at scales below the Hubble radius. The magnetic field provides an additional pressure that can prevent the growth of a given perturbation; however, the magnetic pressure is confined only to the plane orthogonal the field. As a result, the "Jeans length" of the system not only depends on the wavelength of the fluctuation but al… Show more

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Cited by 6 publications
(48 citation statements)
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“…with x i given by (97) with Λ S = 0, or equivalently by (102). If we compare our result with [5], we identify the anisotropic behaviour and we obtain the correct Newtonian limit of [24]. However, our solutions are different and we are unable to explain such discrepancy: we can argue they may have found some sort of average effect, however this is not clear, given the strong anisotropy of the model: the magnetic Jeans wavenumber is present only in one direction, the one with µ = 0.…”
Section: Full Relativistic Casementioning
confidence: 66%
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“…with x i given by (97) with Λ S = 0, or equivalently by (102). If we compare our result with [5], we identify the anisotropic behaviour and we obtain the correct Newtonian limit of [24]. However, our solutions are different and we are unable to explain such discrepancy: we can argue they may have found some sort of average effect, however this is not clear, given the strong anisotropy of the model: the magnetic Jeans wavenumber is present only in one direction, the one with µ = 0.…”
Section: Full Relativistic Casementioning
confidence: 66%
“…While formally the best solution to this problem would be using a two fluid model, with a different equation of state for perturbations, here we will simply drop the relation between v 2 S and w and assume that the perturbed fluid follows a different equation of state with respect to the background fluid. This is correct in the Newtonian approximation and it's in fact the standard way of handling things [39,24], while putting v 2 S = 0 at the end will recover the full covariant value of our calculations for studying pure magnetic effects.…”
Section: Sound Speed and Alfvén Speedmentioning
confidence: 79%
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