2019/12/27 by Ramkishor Sharma, Kandaswamy Subramanian, T. R. Seshadri · 21 citations
Earth and Planetary Sciences · Physics and Astronomy · #Anisotropy #Astrophysics #Cosmic microwave background #Cosmology and Gravitation Theories #Electromagnetic radiation #Electromagnetic spectrum #Geophysics and Gravity Measurements #Gravitational wave #Gravitational wave background #Inflation (cosmology) #Inflaton #Magnetic field #Physics #Pulsar #Pulsars and Gravitational Waves Research #Quantum electrodynamics #Quantum mechanics #Range (aeronautics) #Theoretical physics #Universe #astro-ph.CO #gr-qc
paper · pdf · doi:10.1103/physrevd.101.103526
published in Physical review. D/Physical review. D. 101(10) (American Physical Society) · 25 pages, 5 figures, comments are welcome
arxiv created 2019/12/27 · openalex publication_date 2020/05/21 · arxiv updated 2020/05/27 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Generation of magnetic fields during inflation is a promising mechanism for the origin of the observed large scale magnetic fields in the universe. Among several attempts, a popular model is one where the inflaton and the electromagnetic field are coupled through a coupling function f leading to a term in the Lagrangian density of the form, f2F^\ensuremathμ\ensuremathνF_\ensuremathμ\ensuremathν. A number of potential difficulties with such models have been raised in the literature. In our earlier work, we have suggested viable models of inflationary magnetogenesis which avoid these problems and at the same time can lead to either nonhelical or helical magnetic fields of astrophysical interest. Our models require a low energy scale for inflation and reheating (reheating temperature, TR<104 GeV) and generate a blue spectrum of electromagnetic (EM) field which peaks around the horizon scale of reheating. We show here that the anisotropic stress associated with these EM fields naturally source the production of a stochastic background of Gravitational waves (GW) with frequencies in the range of tens of nano Hertz to milli Hertz. These two extremes of the range can be probed respectively by pulsar timing arrays (PTA) experiments and the upcoming Laser Interferometric Space Array (LISA). The peak value of the GW spectrum energy represented by d\mathrm\ensuremathΩGW/dlnk is 10^\ensuremath-6 for the models which lead to nonhelical primordial fields and 2\ifmmode×\else\texttimes\fi10^\ensuremath-6 for the helical case for TR=100 GeV. In this case the spectrum peaks at a frequency 30 \ensuremathμHz for nonhelical case and at 40 \ensuremathμHz for helical case. These values are obtained when the ratio of EM energy density to the cosmological density at reheating \ensuremathε\ensuremath∼1 and decrease approximately as \ensuremathε2 for smaller values. The amplitude is similar for a lower value of TR, but the frequency at which the GW spectrum peaks decreases as TR. The gravitational waves generated are unpolarized if the EM fields are nonhelical but are circularly polarized for helical primordial fields. If detected in the future these gravitational waves will provide a unique probe of such models of inflationary magnetogenesis.