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| Paper: |
Cosmic Magnetic Fields from Torsion Modes and Massive Photon Inflation |
| Volume: |
488, 8th International Conference of Numerical Modeling of Space Plasma Flows (ASTRONUM 2013) |
| Page: |
57 |
| Authors: |
Garcia de Andrade, L. C. |
| Abstract: |
Earlier Barrow & Tsagas (2008) showed that a slower decay of magnetic fields are present in open Friedmann universes, with traditional Maxwell equations. In their paper magnetic fields of the order of B∼10–33 G which are far below the value required to seed galactic dynamos were obtained. In this paper galactic dynamo seeds of the order of B∼10–23 G are obtained from massive electrodynamics in Einstein–Cartan–Proca (ECP) expanding universe of de Sitter type. Slow decay of magnetic fields in photon-torsion coupling in QED (Garcia de Andrade 2011b) have been recently shown by Garcia de Andrade (2012) also not be able to seed galactic dynamos. Torsion modes are constrained by the field equations. Space-time torsion is shown to be explicitly responsible for the slow decay of cosmic magnetic field. In the absence of massive photon torsion coupling the magnetic field decay is of the order B∼t–3/2, while when torsion is turn on B∼t–1.2. The pure massive-photon-torsion contribution amplifies the magnetic field by Btorsion∼t0.1 which characterizes an extremely slow magnetic dynamo action due to purely torsion gravitational effects. Recently, Barrow et al. (2012) have obtained superadiabatic amplification of B-fields in the Friedmann open cosmology which lies within 10–20 G and 10–12 G which falls very comfortable within limits to seed galactic dynamos. Other simple solutions where B-field decays as B∼a–1, relatively weak photon-torsion coupling approximation. These solutions are obtained for the de Sitter and Friedmann metrics. |
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