TASI lectures on black holes in string theory

By A.W. Peet. 2000

310 citations recorded by the source corpus.

This is a write-up of introductory lectures on black holes in string theory given at TASI-99. Topics discussed include: Black holes, thermodynamics and the Bekenstein-Hawking entropy, the information problem; supergravity actions, conserved quantum numbers, supersymmetry and BPS states, units and duality, dimensional reduction, solution-generating; extremal M-branes and D-branes, smearing, probe actions, nonextremal branes, the Gregory-Laflamme instability; breakdown of supergravity and the Correspondence Principle, limits in parameter space, singularity resolution; making black holes with branes, intersection-ology, explicit d=5,4 examples; string/brane computations of extremal black hole entropy in d=5,4, rotation, fractionation; non-extremality and entropy, the link to BTZ black holes, Hawking radiation and absorption cross-sections in the string/brane and supergravity pictures.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/ad688bf4b7341f710efe2568f9c56432260b652b

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Citations in the corpus

Thermodynamical Aspects of Gravity: New insights (2009, background): “There have also been attempts to compute black hole entropy in different models of quantum gravity [86].”
Aspects of holography for theories with hyperscaling violation (2012, background): “ similar remarks in [14]. 6.1 Black-brane solutions Let us rst review the necessary results on black branes in ten-dimensional supergravity. For more details and references to the literature see e.g. [5, 45]. In 10d string frame, the 24 Dp-black brane solution is ds2 str = 2 f +(ˆ) p f (ˆ) dt + p f ”
Time Dependence of Hawking Radiation Entropy (2013, background): “Interest in black hole information [1, 2, 3, 4, 5, 6, 7, 8, 9, 10, 11, 12, 13, 14, 15, 16, 17, 18, 19, 20, 21, 22, 23, 24, 25, 26, 27, 28, 29, 30, 31, 32, 33, 34, 35, 36, 37, 38, 39, 40, 41, 42, 43, 44, 45, 46, 47, 48, 49, 50, 51, 52, 53, 54, 55, 56, 57, 58, 59, 60, 61, 62, 63, 64, 65, 66, 67, 68, 6”
How far are we from the quantum theory of gravity (2003, background): “magnetic charges are, in appropriate units, equal to their masses. Classical supergravity has BPS states (i.e. classical solutions), among which are black holes whose charges are equal to their masses[145]. These are also called extremal because there is a theorem that the charges cannot exceed thei”
Gravity and the Thermodynamics of Horizons (2003, background): “In standard string theory this is done as follows: There are certain special states in string theory, called BPS states[120], that contain electric and magnetic charges which are equal to their mass.”
M(atrix) Theory: Matrix Quantum Mechanics as a Fundamental Theory (2001, background): “Indeed, it was argued by Polchinski (1999) that the size of the bound-state wave function of N D0-branes will grow at least as fast as N1/3.”
Global structure of five-dimensional fuzzballs (2013, background): “It is fairly common to go to a system of units in which the five-dimensional Planck length, 5, is unity and this means (see, for example, [98, 99]): G5 = π 4 .”
Black holes, black rings and their microstates (2007, background): “(See, for example, [63] in order to get the charge normalizations precisely correct.”
Lectures on black holes, topological strings and quantum attractors (2006, unknown): “to [21, 22, 23, 24] for more details and references.”
The Holographic principle (2002, background): “Recent developments in string theory have led to models of limited classes of black holes in which the microstates can be identified and counted (Strominger and Vafa, 1996; for a review, see, e.g., Peet, 2000).”
On universality of stress-energy tensor correlation functions in supergravity (2004, background): “10) The zero law of black hole (brane) thermodynamics requires [19] that the surface gravity (or equivalently the temperature) is constant over the horizon for a stationary black hole.”
Gravity and the thermodynamics of horizons (2005, background): “In standard string theory this is done as follows: There are certain special states in string theory, called BPS states [120], that contain electric and magnetic charges which are equal to their mass.”
The evolution of unstable black holes in anti-de Sitter space (2000, background): “Finally, it is worth pointing out that the string theory program of computing black hole entropy via a microscopic state count in a field theory dual (see for example [46], or [47] for a review) has proved hard to extend past the boundaries of thermodynamic stability.”