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Hairy Holes

Hairy Holes

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The continuum-fitting and the iron line methods are leading techniques capable of probing the spacetime geometry around astrophysical black hole candidates and testing the no-hair theorem. Firstly Hesleden Dene is a very steep sided valley, incised into the Mag limestone by the melt waters of the last ice age, crossing the stream at this time of year is difficult, but not entirely impossible so cold and soggy footed we started the 8 meter(ish) climb up the cliff face to the hole.

Mass and spin are the first two multipole moments of the Kerr spacetime and completely determine all other moments. The last few years have witnessed further progress on several fronts, including the accurate numerical evolution of the gravitational field equations, which now allows highly nonlinear phenomena to be tamed. Robinson, under the additional hypothesis of non-degenerate event horizons and the technical, restrictive and difficult-to-justify assumption of real analyticity of the space-time continuum. Black holes have long been considered the perfect laboratory to study how to merge Einstein’s theory of general relativity with quantum mechanics,” said Professor Xavier Calmet, a physicist at the University of Sussex.

All other variations in the black hole will either escape to infinity or be swallowed up by the black hole. First, there are solutions with proportional metrics, which are the same as in General Relativity with a cosmological term, which can be positive, negative or zero. They are also hugely important as places where new physics, such as an extension to Einstein’s theory of general relativity, might be on display.

The latter case involves a conformally coupled scalar field as well as an electromagnetic field and the (primary) hair black holes thus obtained. In this paper we classify the obstructions of symmetry inheritance by the scalar fields, both real and complex, and look more closely at the special cases of stationary and axially symmetric spacetimes. We review the black hole (BH) solutions of the ghost-free massive gravity theory and its bimetric extension, and outline the main results on the stability of these solutions against small perturbations. As supplementary material to this paper we make available numerical data files for the sample of reference solutions discussed, for public use (see stacks. Physicist John Archibald Wheeler expressed this idea with the phrase "black holes have no hair", [1] which was the origin of the name.After climbing up it turned out to be (after a promising looking entrance) 5meters 40cm deep although in the alcove at the back are what appear to be two slip rifts running off east and west which can be followed for about 2 meters before becoming too tight.

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