Bulletin of the American Physical Society
2014 Annual Fall Meeting of the APS Prairie Section
Volume 59, Number 19
Friday–Saturday, November 21–22, 2014; Monmouth, Illinois
Session D1: Astrophysics, Cosmology and Astronomy I |
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Room: CSB 100 - Pattee Auditorium |
Saturday, November 22, 2014 12:45PM - 1:21PM |
D1.00001: The Cosmology of Primordial Black Holes Invited Speaker: James Chisholm Ever since their theoretical ``discovery'' more than 40 years ago, black holes created in the earliest stages of the universe with masses below the Chandrasekhar limit -- or Primordial Black Holes (PBHs) -- have continued to be investigated for their influence in a number of cosmological contexts. In this talk, I will review some of the ways PBHs have been invoked in the past to resolve cosmological mysteries, as well as mechanisms for their continued influence in the universe today. [Preview Abstract] |
Saturday, November 22, 2014 1:21PM - 1:33PM |
D1.00002: The Early University (f$^2$ FF) Model of Primordial Magnetic Field at Large Field Inflation Anwar AlMuhammad Primordial magnetic fields (PMF) are detected in almost all astrophysical systems and scales from planets to superclusters of galaxies. They also have been detected in very low density intergalactic medium with $B_{0} >10^{-16}\mathrm{G}$. The simple inflation model, $(f^{2}FF)$ becomes more attractive because it leads to a scale invariant PMF. Recently, BICEP2 reported the detection of the tensor mode (B-mode) of the polarization of temperature anisotropy in CMB. The tensor to scalar ratio reported was $r=0.2_{-0.05}^{+0.07} $, which, if confirmed, raises the scale of inflation to GUT scale, $\rho_{\mathrm{GUT}}^{1/4}\sim 10^{16}$ GeV. The chaotic inflationary models, such as large field inflation (LFI) fit the new result more than the standard models. We compute both magnetic and electric spectra generated by the $f^{2}FF$ model in the LFI for all possible values of model parameter, $p$. We show that the necessary scale invariance property of PMF cannot be obtained in LFI under the first order of slow roll limits. Furthermore, if the limits were released to achieve the scale invariance, the model would suffer from backreaction problems. [Preview Abstract] |
Saturday, November 22, 2014 1:33PM - 1:45PM |
D1.00003: Inflation and Blowing to eliminate irregularities Ahmad Al-Tahan We determine that it is possible for cosmological inflation to occur without leaving behind irregularities and unresolved infinite results. We suggest that inflation should be followed by a blowing of matter instead of a slow expansion, which would be a viable way of forming galaxies and resolving the issue of having everlasting irregularities left from inflation. We accordingly propose a late inflation of the Gravity Attraction Sky--the center of gravity attraction in the universe--to reduce irregularities, increase the influence of gravity upon the matter and bring the universe energies into zero balance. We also suggest that fast, late inflation ended with expansion that maintained the zero-energy balance. Expansion was followed by acceleration, a process related to the influence of the expansion of the Gravity Attraction Sky on matter. Acceleration relating to the flow of matter toward the Gravity Attraction Sky increases each time matter approaches the Gravity Attraction Sky. The increase in acceleration would lead to the end of the universe because of its increasing mass. We suggest that dark energy is a kind of wind energy that initiated and decayed when matter and anti-matter annihilated. The results, should help scientists resolve several obstacles. [Preview Abstract] |
Saturday, November 22, 2014 1:45PM - 1:57PM |
D1.00004: Fractal boundaries in chaotic scattering of charged particles from a magnetic neutral line field Richard Martin, Daniel Holland, Jamie Svetich In this talk we examine chaotic scattering of charged particles in magnetotail-like fields in the Earth's magnetosphere. We focus on a two-dimensional magnetic neutral line field and compare results with the better studied magnetic field reversal current sheet field. Both of these Hamiltonian systems exhibit chaotic scattering over a wide range of parameter values. In the current sheet there is a well defined energy resonance that governs the dynamics, and we show that the neutral line model has no such resonance. We investigate the fractal behavior of the final state exit region boundaries when particles are injected far from the neutral line or field reversal region. Both models have fractal exit region boundaries, and we compare their behavior. [Preview Abstract] |
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