From Osher Doctorow
Li-Xin Li's (1997) paper will be somewhat clearer if you look up
"Primordial fluctuations,"
http://en.wikipedia.org/wiki/Primordial_fluctations, last modified 31
May 2005, and in the same http except for the last expression "Quantum
fluctuation," "Spectral density," "Cosmic inflation," "Inflation."
For example, backslash inflaton replaces backslash Primordial
underscore fluctuations to access that site, or just use the name as
keywords.
Another very useful reference is Steven Weinberg's (1972) Gravitation
and Cosmology Principles and Applications of the General Theory of
Relativity, Wiley: N.Y. under the following topics especially:
A. Disperson, Disperson Relation (pp. 503-506, 563, etc.)
B. Fluctuations, Protogalactic Fluctuations, pp. 565, 504, 518-519,
498, 522
C. Perturbations, Small Perturbations, pp. 562 ff (and following
pages), 581-82, 583
D. Disturbances, 564
E. Flux, 508 (see p. 519 in connection with this), 453
F. Dissipation, 579, 593, etc.
As you can guess, ultimately Li and Weinberg ascribe expansion of the
universe and related processes to the Heisenberg Uncertainty Principle
(HUP).
The PI (Probable Influence) theory regards HUP as at most an
approximation under certain microscopic conditions to
Expansion-Contraction in the vacuum(s) and other scenarios and to the
built-in difference (which is especially apparent at microscopic
levels) between the two-point or more accurately point-neighborhood
nature of momentum and the one-point or one-little-string nature of
position. Analogously for energy and time.
Osher Doctorow
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