By Spiros Cotsakis (auth.), Manolis Plionis, Spiros Cotsakis (eds.)
ISBN-10: 9401006229
ISBN-13: 9789401006224
ISBN-10: 9401039313
ISBN-13: 9789401039314
The choice of shows during this quantity represents a lovely stability among the wealthy matters into which cosmology has matured over the last a long time.
First, the contributions of the `Architects' talk about fundamentalcosmology, targeting the topology and geometry of our Universe and the elemental actual legislation and tactics within the Very Early Universe.
Next, the `Constructors' speak about the final word awareness of the cosmic framework with the new determinations of the cosmological parameters which signify the Friedmann-Robertson-Walker metric.
Finally, the `Interior Decorators' look after the cosmic infrastructure, a few focusing on the paintings of gravity, a few answerable for the formation of the megaparsec cosmic constitution whereas others are heroically attempting to mix gravitational, hydrodynamic, radiative, stellar, and various different dissipative methods right into a brave try out in the direction of realizing the lighting within the cosmos.
Read Online or Download Modern Theoretical and Observational Cosmology: Proceedings of the 2nd Hellenic Cosmology Meeting, held in the National Observatory of Athens , Penteli, 19–20 April 2001 PDF
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Extra info for Modern Theoretical and Observational Cosmology: Proceedings of the 2nd Hellenic Cosmology Meeting, held in the National Observatory of Athens , Penteli, 19–20 April 2001
Sample text
Covariantly, 49 Geometrical Aspects of CosmicMagnetic Fields gravity waves are described via the electric (Eab ) and the magnetic (Hab) parts of the Weyl tensor [8]. Their magnitudes, E 2 = EabEab /2 and H 2 = HabHab /2, provide a measure of the wave's energy density and amplitude. Given that H ab = curluab, we can simplify the problem by replacing the magnetic Weyl tensor with the shear. Note that the field couples to gravitational radiation directly via the anisotropic magnetic stresses, which affect the propagation of both Eab and Uab [9].
According to Eq. (6), the magnetocurvature effects also depend on the material component of the universe. e. for 0 ~ w ~ 1) the most intriguing cases occur in positively curved spaces. e. for stiff matter) the Alfven speed grows as c~ ex: a2 and the magneto-curvature term in Eq. (6) becomes time-independent. In this case the field acts as an effective positive cosmological constant. For radiation and dust, on the other hand, c~ = const. and c~ ex: a-I respectively. In these cases the magnetocurvature term is no longer time independent but drops with time mimicking a time-decaying quintessence [5].
The mass M of the field will be here considered to be arbitrarily small and will be kept different from zero. This is nice, both for computational reasons as well as for physical ones, since a very tiny mass for the field can never be excluded. Some comments about the choice of our model are in order. The first seems obvious: the coupling of the scalar field to gravity should be considered. The differential operator in our curved spacetime will be: (27) as corresponds to a massive scalar field of mass M, being R the curvature scalar and the coupling constant = 1/6 for conformal coupling).
Modern Theoretical and Observational Cosmology: Proceedings of the 2nd Hellenic Cosmology Meeting, held in the National Observatory of Athens , Penteli, 19–20 April 2001 by Spiros Cotsakis (auth.), Manolis Plionis, Spiros Cotsakis (eds.)
by Donald
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