Consistency relation for cosmic magnetic fields

Jain, Rajeev Kumar; Sloth, Martin S.

doi:10.1103/physrevd.86.123528

Cited by 50 publications

(82 citation statements)

References 35 publications

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“…It is also interesting to notice that (4.46) is in agreement with previous results found in [58,59] in the squeezed limit, i.e. when k 1 → 0.…”

Section: Three Point Functionsupporting

confidence: 81%

“…Moreover, in the squeezed limit when all the modes are in the super horizon regime, and we were able to derive the relation (4.49) for the cross correlation of scalar and vectors with a power law coupling to the conformal time. This result is related with the consistency relation obtained in [58,59] for the cross correlator in the f (φ)F 2 model. The main shortcoming of the method followed here is that we can't obtain the suppression factor appearing in the squeezed limit, since, as we said before, the symmetry analysis gives us the general structure of the correlators up to amplitude factors.…”

Section: Conclusion and Final Remarksmentioning

confidence: 83%

“…The interest for those models has been diverse and it has evolved over the years. It is worthwhile to mention the Ratra model [32], which has a rich and interesting phenomenology in the context of primordial magnetogenesis scenario [36,[57][58][59][60] and later used as a source of sizable statistical anisotropies which doesn't dilute with the inflationary evolution [29,[33][34][35]37]. Aside of this, there is a rich literature about models whit an axion/pseudoscalar coupling of the form φFF which allows for interesting phenomenology and source of nonvacuum gravitational waves, chiral gravitational waves, large tensor non-gaussianities among other interesting effects [38,47,49,52,55].…”

Section: A Parity Violating Scalar-vector Inflationary Modelmentioning

confidence: 99%

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de Sitter symmetries and inflationary correlators in parity violating scalar-vector models

Almeida

Motoa-Manzano

Valenzuela-Toledo

2017

J. Cosmol. Astropart. Phys.

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Abstract. In this paper we use conformal field theory techniques to constrain the form of the correlations functions of an inflationary scalar-vector model described by the interaction term f 1 (φ)F µν F µν + f 2 (φ)F µν F µν . We use the fact that the conformal group is the relevant symmetry group acting on super horizon scales in an inflationary de Sitter background. As a result, we find that super horizon conformal symmetry, constraints the form of the coupling functions f 1 , f 2 to be homogeneous functions of the same degree. We derive the general form of the correlators involving scalar and vector perturbations in this model and determine its squeezed limit scaling behaviour for super horizon scales. The approach followed here is useful to constraint the shape of scalar-vector correlators, and our results agree with recent literature on the subject, but don't allow us to determine amplitude factors of the correlators.

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“…It is also interesting to notice that (4.46) is in agreement with previous results found in [58,59] in the squeezed limit, i.e. when k 1 → 0.…”

Section: Three Point Functionsupporting

confidence: 81%

Section: Conclusion and Final Remarksmentioning

confidence: 83%

Section: A Parity Violating Scalar-vector Inflationary Modelmentioning

confidence: 99%

See 1 more Smart Citation

de Sitter symmetries and inflationary correlators in parity violating scalar-vector models

Almeida

Motoa-Manzano

Valenzuela-Toledo

2017

J. Cosmol. Astropart. Phys.

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“…Such magnetic fields could be of cosmological origin [16][17][18][19][20][21] or they could be related to some source that can demonstrate a complex structure in the vicinity of field source, but at large distances, their character can be simple and close to a homogeneous magnetic field (see Fig. 1) -for simplicity, such magnetic fields are considered to be asymptotically uniform as discussed in [22].…”

Section: Introductionmentioning

confidence: 99%

Acceleration of the charged particles due to chaotic scattering in the combined black hole gravitational field and asymptotically uniform magnetic field

2016

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To test the role of large-scale magnetic fields in accretion processes, we study the dynamics of the charged test particles in the vicinity of a black hole immersed into an asymptotically uniform magnetic field. Using the Hamiltonian formalism of the charged particle dynamics, we examine chaotic scattering in the effective potential related to the black hole gravitational field combined with the uniform magnetic field. Energy interchange between the translational and oscillatory modes of the charged particle dynamics provides a mechanism for charged particle acceleration along the magnetic field lines. This energy transmutation is an attribute of the chaotic charged particle dynamics in the combined gravitational and magnetic fields only, the black hole rotation is not necessary for such charged particle acceleration. The chaotic scatter can cause a transition to the motion along the magnetic field lines with small radius of the Larmor motion or vanishing Larmor radius, when the speed of the particle translational motion is largest and it can be ultra-relativistic. We discuss the consequences of the model of ionization of test particles forming a neutral accretion disc, or heavy ions following off-equatorial circular orbits, and we explore the fate of heavy charged test particles after ionization where no kick of heavy ions is assumed and only the switch-on effect of the magnetic field is relevant. We demonstrate that acceleration and escape of the ionized particles can be efficient along the Kerr black hole symmetry axis parallel to the magnetic field lines. We show that a strong acceleration of the ionized particles to ultra-relativistic velocities is preferred in the direction close to the magnetic field lines. Therefore, the process of ionization of Keplerian discs around the Kerr black holes can serve as a model of relativistic jets. a

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“…One therefore gets b NL = O(f ′ /f H) [34,35]. In the squeezed limit, with the parametrization of the coupling of the form f (φ(τ )) ∼ τ n , the index n can be related to the spectral index of the magnetic field power spectrum n B = (4−2n), implying b NL = (n B − 4).…”

Section: Violation Of the Cosmological Magnetohydrodynamics Consistenmentioning

confidence: 99%

Testing the origin of cosmological magnetic fields through the large-scale structure consistency relations

Berger

Kehagias

Riotto

2014

J. Cosmol. Astropart. Phys.

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We study the symmetries of the post-recombination cosmological magnetohydrodynamical equations which describe the evolution of dark matter, baryons and magnetic fields in a self-consistent way. This is done both at the level of fluid equations and of Vlasov-Poisson-Maxwell equations in phase space. We discuss some consistency relations for the soft limit of the (n + 1)-correlator functions involving magnetic fields and matter overdensities. In particular, we stress that any violation of such consistency relations at equal-time would point towards an inflationary origin of the magnetic field.

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Consistency relation for cosmic magnetic fields

Cited by 50 publications

References 35 publications

de Sitter symmetries and inflationary correlators in parity violating scalar-vector models

de Sitter symmetries and inflationary correlators in parity violating scalar-vector models

Acceleration of the charged particles due to chaotic scattering in the combined black hole gravitational field and asymptotically uniform magnetic field

Testing the origin of cosmological magnetic fields through the large-scale structure consistency relations

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