New PDF release: Cosmological Milestones and Gravatars - Topics in General

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This singular point referred to as the big bang had an infinite density of matter and an infinite curvature of spacetime. The value of the Hubble parameter changes over time either increasing or decreasing depending on the sign of the deceleration parameter : q=− a¨ a . 43) The deceleration parameter measures the rate of change of the rate of expansion. Different values, or ranges of values, of q0 correspond to different cosmological models. In principle, it should be possible to determine the value of q0 observationally.

Recently it has been speculated that in an expanding FLRW universe a curvature singularity may occur at a finite time before a “Big Crunch” for matter contents that satisfy both weak and strong energy conditions. This family of models has been further enlarged, and the same sort of behavior has also been found in inhomogeneous models [6, 7]. We shall define the scale factor near a sudden singularity using the generalized power series expansion. Definition 4. Let the time of the sudden singularity, if one occurs, be t⊖ (past or future).

47) where M⊙ is the solar mass and h is the present day normalized Hubble expansion rate. 37), we can then write: Ω−1= k . 48) The sign of k is therefore determined by whether the energy density parameter Ω is greater than, equal to, or less than one. 49) The density parameter, then, indicates which of the three Robertson-Walker geometries describes our universe. 02. 5 6 See S. Eidelman et al. from the Particle Data Group [29] for recent measurement values. See S. Eidelman et al. from the Particle Data Group [29] for recent measurement values.

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Cosmological Milestones and Gravatars - Topics in General Relativity [thesis] by C. Cattoen

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