Get An Introduction to Black Holes, Information And The String PDF

By Leonard Susskind

ISBN-10: 9812560831

ISBN-13: 9789812560834

Over the past decade the physics of black holes has been revolutionized via advancements that grew out of Jacob Bekenstein's awareness that black holes have entropy. Steven Hawking raised profound concerns about the lack of details in black gap evaporation and the consistency of quantum mechanics in a global with gravity. for 2 many years those questions wondered theoretical physicists and at last resulted in a revolution within the method we predict approximately area, time, subject and data. This revolution has culminated in a outstanding precept referred to as "The Holographic Principle", that's now an immense concentration of realization in gravitational learn, quantum box thought and uncomplicated particle physics. Leonard Susskind, one of many co-inventors of the Holographic precept in addition to one of many founders of String idea, develops and explains those suggestions.

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Additional resources for An Introduction to Black Holes, Information And The String Theory Revolution: The Holographic Universe

Example text

Notice that null geodesics are vertical after the shell crosses the horizon and essentially at 45o prior to that crossing. These light rays are called the generators of the horizon. Singularity forms XXXXXXXXXXXXXXXXXXXXXXXXXXXXXXXXXXXXXXXXXXXXXXXXXXX The Schwarzschild Black Hole 21 Horizon Shell crosses Horizon Shell of radially moving light-rays Horizon Forms Fig. 7 The horizon as family of null geodesics Fidos and Frefos and the Equivalence Principle In considering the description of events near the horizon of a static black hole from the viewpoint of an external observer[1], it is useful to imagine space to be filled with static observers, each located at a fixed (r, θ, φ).

25 indicates that some of the s-wave particles will easily escape to infinity. Unless the black hole is kept in equilibrium by incoming radiation it will lose energy to its surroundings. Particles of angular momenta higher than s-waves cannot easily escape because the potential barrier is higher than the thermal scale. The black hole is like a slightly leaky cavity containing thermal radiation. Most quanta in the thermal atmosphere have high angular momenta and reflect off the walls of the cavity.

Particles of angular momenta higher than s-waves cannot easily escape because the potential barrier is higher than the thermal scale. The black hole is like a slightly leaky cavity containing thermal radiation. Most quanta in the thermal atmosphere have high angular momenta and reflect off the walls of the cavity. A small fraction of the particles carry very low angular momenta. For these particles, the walls are semi-transparent and the cavity slowly radiates its energy. This is the process first discovered by Hawking and is referred to as Hawking radiation.

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An Introduction to Black Holes, Information And The String Theory Revolution: The Holographic Universe by Leonard Susskind


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