On the Relevance of the Thermal Scalar

Abstract

We discuss near-Hagedorn string thermodynamics in general spacetimes using the formalism of the thermal scalar. Building upon earlier work by Horowitz and Polchinski, we relate several properties of the thermal scalar field theory (i.e. the stress tensor and U(1) charge) to properties of the highly excited or near-Hagedorn string gas. We apply the formulas on several examples. We find the pressureless near-Hagedorn string gas in flat space and a non-vanishing (angular) string charge in $Ad{S}_3$. We also find the thermal stress tensor for the highly excited string gas in Rindler space.

arXiv comment36 pages, v2: section on correlators rewritten and clarifications added, matches published version

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• Stringy Horizons and UV/IR Mixing
• Revisiting noninteracting string partition functions in Rindler space
• Cloud of strings in f(R) gravity
• Effective field theory for closed strings near the Hagedorn temperature
• String Theory in Polar Coordinates and the Vanishing of the One-Loop Rindler Entropy
• Hagedorn String Thermodynamics in Curved Spacetimes and near Black Hole Horizons
• On the Stringy Hartle-Hawking State
• Size scaling of self gravitating polymers and strings
• Fluid model of a black hole-string transition