The primordial magnetic field generated at large field inflation, natural inflation, and R2-inflation by f2FF model

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dc.contributor.advisorSchlegel, Eric M.
dc.contributor.advisorLopez-Mobilia, Rafael
dc.contributor.authorAlMuhammad, Anwar Saleh
dc.contributor.committeeMemberPackham, Chris
dc.contributor.committeeMemberMarucho, Marcelo
dc.contributor.committeeMemberTavernini, Lucio
dc.date.accessioned2024-01-26T20:58:45Z
dc.date.available2024-01-26T20:58:45Z
dc.date.issued2015
dc.descriptionThis item is available only to currently enrolled UTSA students, faculty or staff. To download, navigate to Log In in the top right-hand corner of this screen, then select Log in with my UTSA ID.
dc.description.abstractLarge scale magnetic fields seem to be present in almost all astrophysical systems and scales from planets to superclusters of galaxies and in very low density intergalactic media. The upper limit of primordial magnetic fields (PMF) has been set by recent observations by the Planck observatory (2015) to be of the order of a few nG. The simple model ${f^2}FF$ used to generate the PMF during the inflation era. It is based on the breaking of conformal symmetry of electromagnetism during inflation. It is attractive because it is stable under perturbations and leads to a scale invariant PMF. However, it may suffer from two problems: Backreaction and strong coupling. In the first case, the electromagnetic energy may exceed the energy of inflation, ${rho _{{rm{Inf}}}}$. In the second case, the effective electric charges become excessively large if we want to retrieve the standard electromagnetism at the end of inflation. In this research, we investigate the generation of PMF under three different models of inflation in order to avoid the backreaction problem. We compute magnetic and electric spectra generated by the ${f^2}FF$ model in the context of large field inflation (LFI), natural inflation (NI) and ${R^2}$-inflation, for all possible values of model parameters for de Sitter and power law expansion of inflation. The results of the research show that the scale invariant PMF can be generated in these models and the problem of backreaction may be avoided in some observational ranges. ${R^2}$-inflation, which is preferred by the recent results of Planck 2015, we calculate the upper of the scale invariant PMF generated by ${f^2}FF$ and in turns we find that the upper limit of present magnetic field, ${B_0} < 8.058 times {10^{ - 9}}{rm{G}}$. It is in the same order of magnitude of PMF, reported by Planck, 2015.
dc.description.departmentPhysics and Astronomy
dc.format.extent146 pages
dc.format.mimetypeapplication/pdf
dc.identifier.isbn9781339308456
dc.identifier.urihttps://hdl.handle.net/20.500.12588/2586
dc.languageen
dc.subjectCosmology
dc.subjectInflation
dc.subjectPrimordial Magnetic Field
dc.subject.classificationTheoretical physics
dc.subject.lcshCosmic magnetic fields -- Mathematical models
dc.titleThe primordial magnetic field generated at large field inflation, natural inflation, and R2-inflation by f2FF model
dc.typeThesis
dc.type.dcmiText
dcterms.accessRightspq_closed
thesis.degree.departmentPhysics and Astronomy
thesis.degree.grantorUniversity of Texas at San Antonio
thesis.degree.levelDoctoral
thesis.degree.nameDoctor of Philosophy

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