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Titlebook: Gauge Theory and the Early Universe; P. Galeotti,David N. Schramm Book 1988 Kluwer Academic Publishers 1988 Cosmology.Dark matter.Gravity.

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11#
發(fā)表于 2025-3-23 10:23:09 | 只看該作者
Monopoles and Axions in an Inflationary Universe,n S0(10) model, for example, magnetic monopoles with mass ~ 10. – 10. GeV can occur at a level which is experimentally detectable. The topologically unstable string - wall system of axion models provides an important source of density fluctuations as a consequence of inflation.
12#
發(fā)表于 2025-3-23 16:01:30 | 只看該作者
13#
發(fā)表于 2025-3-23 20:21:11 | 只看該作者
Constraints on the Geometry of the 5th dimension in cosmological solutions of Five dimensional Rela the t,? submanifold as a consequence of the field equations. This justifies the usual assumption that the geometry of the 5th coordinate is a circle. It is shown they are equivalent to the Lorenz - Petzold type (ix) solutions.
14#
發(fā)表于 2025-3-24 01:36:30 | 只看該作者
15#
發(fā)表于 2025-3-24 02:44:56 | 只看該作者
16#
發(fā)表于 2025-3-24 08:32:22 | 只看該作者
https://doi.org/10.1007/978-1-349-11801-4itational field,I calculate the time-evolution of the cosmic scale factor and of the scalar field in the case of a λ?. theory,in order to understand when a λ?. theory is able to drive inflation.Some new topics are mentioned,too.
17#
發(fā)表于 2025-3-24 11:26:16 | 只看該作者
Cosmology and Extra Dimensions,However, if the big bang is extrapolated back to the Planck time, then the characteristic size of . internal and external dimensions were the same, and the internal dimensions may have had a more direct role in the dynamics of the evolution of the Universe. This chapter presents some speculations about the role of extra dimensions in cosmology.
18#
發(fā)表于 2025-3-24 14:54:22 | 只看該作者
19#
發(fā)表于 2025-3-24 20:59:42 | 只看該作者
20#
發(fā)表于 2025-3-25 02:31:34 | 只看該作者
: Australianising HBO-Style Television? connected with the new ideas and developments in the other field. Roughly speaking, many different subdisciplines of physics seem to converge in cosmology, the study of the early evolution of the universe. The range of parameters (dimensions, temperatures, densities, etc..) to be taken into account
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