Black Holes, Gravitational Radiation and the Universe: by B. Carter (auth.), Bala R. Iyer, Biplab Bhawal (eds.)

By B. Carter (auth.), Bala R. Iyer, Biplab Bhawal (eds.)

Our esteemed colleague C. V. Vishveshwara, popularly often called Vishu, grew to become sixty on sixth March 1998. His colleagues and good wishers felt that it'd be acceptable to rejoice the get together by way of bringing out a quantity in his honour. these folks who've had the nice fortune to understand Vishu, understand that he's specified, in a category by way of himself. Having been given the privilege to be the volume's editors, we felt that we should always test anything various during this endeavour. Vishu is among the renowned relativists from India whose pioneer­ ing contributions to the reviews of black holes is universally recognized. He used to be a pupil of Charles Misner. His Ph. D. thesis at the balance of the Schwarzschild black gap, coordinate invariant characterisation of the sta­ tionary restrict and occasion horizon for Kerr black holes and next seminal paintings on quasi-normal modes of black holes have handed directly to turn into the beginning issues for certain mathematical investigations at the nature of black holes. He later labored on different features concerning black holes and compact gadgets. a lot of those issues have matured over the past thirty years. New points have additionally built and develop into present components of full of life study curiosity. not are black holes, ultracompact gadgets or occasion horizons mere idealisations of mathematical physicists yet concrete entities that astrophysicists realize, degree and search for. Astrophysical facts is mounting up gradually for black holes.

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Extra info for Black Holes, Gravitational Radiation and the Universe: Essays in Honor of C.V. Vishveshwara

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46], account was taken of all smooth, spherically symmetric Euclidean geometries satisfying the given boundary conditions, but not necessarily being classical solutions. In the calculation of the partition function, the contribution of each geometry was determined by the value of its classical action, and many geometries could be shown to contribute with the same value. After the classical constraints were imposed, it was found that the partition function could be written as a single ordinary integral in a quantity determined by the size of the black hole horizon.

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