Download An Introduction to Black Holes, Information And The String by Leonard Susskind PDF

By Leonard Susskind

During the last decade the physics of black holes has been revolutionized via advancements that grew out of Jacob Bekenstein's consciousness that black holes have entropy. Steven Hawking raised profound concerns in regards to the lack of info in black gap evaporation and the consistency of quantum mechanics in a global with gravity. for 2 a long time those questions wondered theoretical physicists and finally ended in a revolution within the manner we expect approximately house, time, topic and data. This revolution has culminated in a amazing precept referred to as ''The Holographic Principle'', that is now a massive concentration of consciousness in gravitational learn, quantum box conception and straightforward particle physics. Leonard Susskind, one of many co-inventors of the Holographic precept in addition to one of many founders of String concept, develops and explains those suggestions

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

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There are two viewpoints we can adopt toward the description of the particle’s motion. The first is the viewpoint of the Fidos who are permanently stationed outside the black hole. It is a viewpoint which is also useful to a distant observer, since any observation performed by a Fido can be communicated to distant observers. According to this viewpoint, the particle never crosses the horizon but asymptotically approaches it. The second viewpoint involves freely falling observers (FREFOS) who follow the particle as it falls.

It is composed of a family of light rays or null geodesics, passing through each space-time point on the horizon. 12. 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).

7, that is it coincides with the future horizon of the final black hole geometry and is therefore found at r = 2M G. On the other hand, the horizon also extends into the Region A where the metric is just that of flat space-time. In this region the value of r on the horizon grows from an initial value r = 0 to the value r = 2M G at the shell. It is evident from this discussion that the horizon is a global and not a local concept. In the Region A no local quantity will distinguish the presence of the horizon whose occurence is due entirely to the future collapse of the shell.

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