On the exponential decrease of the “cosmological constant” in the super-early Universe

Abstract

Cosmological consequences of the Poincare-Weyl gauge theory of gravity are considered. A generalized cosmological constant depending from the Dirac scalar field is introduced. The stage of a super-early scale invariant universe is considered. It is shown that while the scale factor sharply increases and demonstrates inflationary behavior, the generalized cosmological constant decreases sharply from a huge value at the beginning of the Big Bang to an extremely small value in the modern era, which solves the well-known “cosmological constant problem”.

The Solution of the Cosmological Constant Problem: The Cosmological Constant Exponential Decrease in the Super-Early Universe

“…The theory constructed is applicable to the super-early stage of a homogeneous Universe with the FRW metrics with a scale factor () at . We obtain two equations, (18) and (19), and using the numerical integration, we obtain the sharp exponential decrease of the effective cosmological constant 2 0   at small t and the exponential increase of the scale factor (Figure 1 and Figure 2) [32]. In the proposed theory, the inflation problem acquires new features: inflation becomes scale-invariant and the Weyl-Dirac scalar field becomes the infraton.…”

“…This requirement determines the value of the constant С . The result of numerical integration of the system of equations (18) and (19) with the boundary condition (20) is presented graphically in [32], where can be seen for small and large times t the inflationary behavior of the scale factor () at , as well as for small times t a sharp exponential decrease in the effective cosmological…”

Strongly Violated Scale Invariance of Space-Time (Quantum-Mechanical Aspect)

“…В работах [14][15][16][17] было найдено космологическое решение для сверхранней Вселенной, в котором через крайне малое время после Большого взрыва (регулируемое свободными параметрами теории) огромная величина эффективной космологической постоянной (энергии вакуума) резко экспоненциально спадает и затем все время эволюции Вселенной, медленно уменьшаясь, приближается к своему современному значению (рис. 1).…”