1.1.1 Problem Fine-Tuning (Weinberg, 1987)
Observed value of the cosmological constant ( 10 MPl4 MPl4) is one of the greatest puzzles in theoretical physics. Theoretically, quantum correction of the vacuum energy of elementary particles is predicted to yield O(MPl4) THE(MPl4), creating a mismatch 120 order size with observation values (Weinberg, 1989). This is known as problem fine tuning , which questions why the vacuum energy of the universe is so small but not exactly zero.
1.1.2 Chaotic Inflation and Multiverse Predictions (Linde, 1983)
The chaotic inflation model introduces a scalar field inflaton ( ) with simple potential V()n V()n, where is the initial condition is random in different regions of space-time (Linde, 1983). The resulting exponential expansion gives rise to multiverse, a collection of "bubble universes" with different laws of physics. In this framework, can vary between bubbles as a stochastic consequence of the initial inflaton conditions (Linde, 1986).
String Theory Landscape as a Source of Variation (Bousso-Polchinski, 2000) .
String theory predicts landscape cosmological by 10 vacuum states stable through an extra-dimensional compactification mechanism (Bousso & Polchinski, 2000). Every empty correspond to different values of determined by quantum numbers flux (in ni):=012i=1Nni2qi2, L=L021i=1Nni2qi2, with qi. qi is the effective load flux. These discrete variations provide the mathematical basis for the distribution of in the multiverse.
1.2 Research Gaps
Although the three concepts above have been developed independently, there is no integrated model that:
1. Integrating chaotic inflation dynamics with variations in landscape wire theory mathematically rigor.
2. Derive the probability distribution from first principles (first principles), combines inflaton quantum fluctuations and anthropic selection.
3. Provides numerical simulation protocols that connect string theory parameters (eg: qi qi, N N) with cosmological observations.
Previous studies tend to be fragmented:
a Analysis of chaotic inflation (Vilenkin, 1983) does not include structure landscape.
b Model landscape (Susskind, 2003) ignores the stochastic dynamics of inflation.
