Statistics – Computation
Scientific paper
Oct 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...398....1s&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 398, no. 1, p. 1-11.
Statistics
Computation
26
Cosmology, Field Theory (Physics), Universe, Astronomical Models, Computational Astrophysics, Evolution (Development)
Scientific paper
Field theory is used to describe the material content of the universe throughout its entire history, and an oscillating cosmological model without a singularity is presented. The 'cosmological fluid' is described by a single scalar field that undergoes a series of phase transitions, each of which denotes a change in the equation of state of the field. We find that an inflationary equation of state (rho equal to about -p) is required in the early universe if the later epochs are to resemble the standard model. We find that H0 = 33-44 km/s per Mpc is the value of the Hubble parameter at the current epoch that is least sensitive to initial conditions. Unlike most other inflation models, the onset of inflation in our theory is independent of an earlier radiation-dominated era. Instead, inflation arises as a consequence of boundary conditions which are expressed in terms of the fundamental Planck quantities. The heating occurs during inflation, and this imposes a thermodynamic constraint on a more complete theory of matter for the early universe. Inflation continues until a maximum possible physical temperature (the Planck temperature) is attained, at which point a phase transition occurs and the standard model begins. For an arbitrary equation of state, we show that the scalar field potential may be derived from the solution of Riccati's equation. We use this result to find the scalar field Lagrangian for the entire history of the universe.
Cooperstock Fred I.
Starkovich Steven P.
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