Titlebook: Black Holes, Gravitational Radiation and the Universe; Essays in Honor of C Bala R. Iyer,Biplab Bhawal Book 1999 Springer Science+Business

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Lipoma

Champion

多樣

Notes on Black Hole Fluctuations and Back-Reaction,n as a manifestation of a fluctuction-dissipation relation was first proposed by Candelas and Sciama [3, 4]. Even though, as we will soon see, the fluctuations in the thought of these earlier authors are not the correct ones and the relations proposed were not really addressing the back-reaction of

Suggestions

信條

Micro-Structure of Black Holes and String Theory,didates in binary systems and there is also evidence that the matter of galaxies is belched in ‘a(chǎn)ctive galactic nuclei’ which are black holes with a million times the solar mass. Why do black holes occur? The standard answer is gravitational collapse and the existence of black hole solutions in gene

ALERT

Quantum Geometry and Black Holes,rature and a multiple of the area of its event horizon should be identified with its thermodynamic entropy [1]. In this reasoning, he had to use not only general relativity but also quantum mechanics. Indeed, without recourse to the Planck’s constant, ?, the identification is impossible because even

杠桿支點(diǎn)

Black Holes, Global Monopole Charge and Quasi-Local Energy,n: can we get the same solutions from a slightly different and more general equation, which is not the derivative of the original equation? The answer is yes. Take the case of the Schwarzshild solution. It is the unique spherically symmetric solution of the Einstein vacuum equation, .. = 0. It can a

半球

Kinematical Consequences of Inertial Forces in General Relativity,on is an indicator of the characteristic of a body that determines its motion. Whereas according to Newton’s law of motion, a body’s state of rest or of uniform motion does in no way characterise its inertia, any change in this state depends upon its inertia. As the change of state can be recorded o

affluent

Neutron Stars and Relativistic Gravity,tic gravity can be understood as the warping of space-time near any object that has mass. Consider the following examples. In Newtonian gravity, a planet orbits around a star in an ellipse. In relativistic gravity the orbit is not a closed curve; it is approximately an ellipse, whose major axis prec