Our Universe as a Dot to Today

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Just under 13.8 billion years ago, our Universe was an infinitesimally tiny dot. A little less than four hundred thousand years after that however, it had become a hot, dense, highly ionized plasma with a temperature of about 5000 degrees Fahrenheit and a density about 109 times the current value (1). Then, something fascinating happened. The plasma underwent a rapid process of recombination, with protons attaching to electrons to form hydrogen, emitting photons with each reaction, and providing the footprints of the Universe of today (2). One of the most interesting aspects of the study of these early moments has been with regards to the non-uniformity of the Universe. This non-uniformity, or anisotropy as it is called, is reflected in the inhomogeneous structure of today’s Universe. During the moments of recombination, energy density fluctuations due to various proposed causes triggered the scattering of photons. As the Universe expanded, this same inhomogeneity has magnified, meaning that by studying the original scattering in the photosphere during the moments of recombination, the current structure of the Universe can be understood to a large extent (2). That is, essentially, the modern Universe and the microwave background are just “image[s] of the surface of [the] last scattering” which occurred about 378,000 years following the Big Bang (1). Thus, in this paper, I will analyze the nature of the Universe’s elementary particles and photons at the time of recombination and will discuss the possibilities of how one type of scattering known as Compton scattering could be used to help describe the non-uniform structure of the present-day Universe.
The Universe at the time of recombination has been theoretically approximated to ...

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...attering would have affected the dynamics of the recombination Universe, causing distortions which can be seen 13.8 billion years later in the form of a non-uniform cosmos. Studying these dynamics closely can give us a much better idea of why the Universe is structured as it is today and allow us to better hypothesize what we should be looking for when studying deep space and galactic structures. Still however, the manifested effects of CMB distortions are small and NASA’s COBE data were not sensitive enough to detect them. Based on the constraints of the new PIXIE mission, the possibility of reconciling these synthesized theories with the experimental data seems likely (6). As shown in Figure 3, the PIXIE limitations are much are fewer. If not PIXIE, the Planck mission could also serve this goal. Nevertheless, until the data come in, astrophysics can only wait.

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