In perturbatively moduli-stabilized brane-antibrane inflation, a modest fraction of annihilation energy into visible open strings can trigger a Hagedorn phase that suppresses ΔN_eff when the SM throat string scale is comparable or lower.
String Gas Cosmology: Progress and Problems
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abstract
String Gas Cosmology is a model of the evolution of the very early universe based on fundamental principles and key new degrees of freedom of string theory which are different from those of point particle field theories. In String Gas Cosmology the universe starts in a quasi-static Hagedorn phase during which space is filled with a gas of highly excited string states. Thermal fluctuations of this string gas lead to an almost scale-invariant spectrum of curvature fluctuations. Thus, String Gas Cosmology is an alternative to cosmological inflation as a theory for the origin of structure in the universe. This short review focuses on the building blocks of the model, the predictions for late time cosmology, and the main problems which the model faces.
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In a 5D open FRW model, negative curvature sustains tracker-like radion evolution that enables dynamical compactification via Casimir stabilization before 4D inflation dilutes curvature remnants.
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Fire at the Tip of the Throat: Hagedorn Phase after brane-antibrane inflation?
In perturbatively moduli-stabilized brane-antibrane inflation, a modest fraction of annihilation energy into visible open strings can trigger a Hagedorn phase that suppresses ΔN_eff when the SM throat string scale is comparable or lower.
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Curvature-Assisted Dynamical Compactification in a Pre-Inflationary Higher-Dimensional Universe
In a 5D open FRW model, negative curvature sustains tracker-like radion evolution that enables dynamical compactification via Casimir stabilization before 4D inflation dilutes curvature remnants.
- The Hagedorn Temperature as a Nonequilibrium Dynamical Bottleneck in String Thermodynamics