Primordial magnetic fields and causality

By R. Durrer, C. Caprini. 2003

185 citations recorded by the source corpus.

We discuss the implications of causality on a primordial magnetic field. We show that the residual field on large scales is much more suppressed than usually assumed, and that a helical component is even more reduced. Due to this strong suppression, even maximal primordial fields generated at the electroweak phase transition can just marginally seed the fields in clusters, but they cannot leave any detectable imprint on the cosmic microwave background.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/a537f1631f5e9781653472970808f1853f0fd783

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. C. Caprini
2. R. Durrer
3. Andrii Y. Neronov
4. G. Servant
5. M. Hindmarsh
6. Mulham Hijazi
7. R. K. Jain
8. M. Sloth

In Nuclear and High Energy Physics

1. C. Caprini
2. R. Durrer
3. Andrii Y. Neronov
4. M. Hindmarsh
5. G. Servant
6. Mulham Hijazi
7. R. K. Jain
8. M. Sloth

Citations in the corpus

• The stochastic gravitational wave background from turbulence and magnetic fields generated by a first-order phase transition (2009, background): “As previously demonstrated [17, 40], the existence of this causal horizon in a cosmological setting implies that the real-space correlation function of the stochastic velocity field has compact support.”
• Gravitational waves from first order cosmological phase transitions in the Sound Shell Model (2019, background): “[48].”
• Steepest growth of the power spectrum and primordial black holes (2018, background): “For primordial magnetic fields, Durrer and Caprini have shown that the two-point function must scale at least as k(2) at large scales [135].”
• Planck 2015 results: XIX. Constraints on primordial magnetic fields (2015, unknown): “…during inflation (Ratra 1992), with a suitable breaking of conformal invariance of electromagnetism (Turner & Widrow 1988), during phase transitions motivated by particle physics (Vachaspati 1991; Grasso & Riotto 1998), or via other physical processes (Durrer & Caprini 2003; Ichiki et al. 2006).”
• Can slow roll inflation induce relevant helical magnetic fields (2010, background): “Their power spectrum is very blue with B(2)(k) ∝ k(2), and therefore, their amplitude on large scales is far too small [26, 27].”
• Inflationary magnetogenesis without the strong coupling problem (2013, background): “Among the primordial mechanisms, magnetic fields generated during phase transitions can have relevant strength but the correlation lengths are typically too small to explain cosmic magnetic fields [11].”
• Cosmological Magnetic Fields: Their Generation, Evolution and Observation (2013, background): “For more details about this conditions which are simply a consequence of causality together with the fact that B is divergence free, see Durrer and Caprini (2003).”