Quantum strings and black holes

Abstract

The transition between (non supersymmetric) quantum string states and Schwarzschild black holes is discussed. This transition occurs when the string coupling $g^2$ (which determines Newton's constant) increases beyond a certain critical value $g_c^2$. We review a calculation showing that self-gravity causes a typical string state of mass $M$ to shrink, as the string coupling $g^2$ increases, down to a compact string state whose mass, size, entropy and luminosity match (for the critical value $g_c^2\sim (M\sqrt{{\alpha }^{\prime }}{)}^{-1}$) those of a Schwarzschild black hole. This confirms the idea (proposed by several authors) that the entropy of black holes can be accounted for by counting string states. The level spacing of the quantum states of Schwarzschild black holes is expected to be exponentially smaller than their radiative width. This makes it very difficult to conceive (even Gedanken) experiments probing the discreteness of the quantum energy levels of black holes.

11 pages, plenary talk given at the 9th Marcel Grossmann Meeting on Recent Developments in Theoretical and Experimental General Relativity, Gravitation and Relativistic Field Theories, Rome, Italy, 2-9 July 2000

Cited by in corpus (6)

• Brane-Antibrane Systems at Finite Temperature and the Entropy of Black Branes
• The family of regular interiors for non-rotating black holes with $T_0^0=T_1^1$
• The Entropy of the Rotating Charged Black Threebrane from a Brane-Antibrane System
• Black Hole Entropy and Superconformal Field Theories on Brane-Antibrane Systems
• AdS Holography and Strings on the Horizon
• Asymptotically Flat Holography and Strings on the Horizon