Radial motion into an Einstein-Rosen bridge

Details Radial motion into an Einstein-Rosen bridge Radial motion into an Einstein-Rosen bridge

2009-02-11

arxiv.org/abs/0902.1994v3

Phys.Lett.B687:110-113, 2010

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

7 pages; published version

Scientific paper

10.1016/j.physletb.2010.03.029

We consider the radial geodesic motion of a massive particle into a black hole in isotropic coordinates, which represents the exterior region of an Einstein-Rosen bridge (wormhole). The particle enters the interior region, which is regular and physically equivalent to the asymptotically flat exterior of a white hole, and the particle's proper time extends to infinity. Since the radial motion into a wormhole after passing the event horizon is physically different from the motion into a Schwarzschild black hole, Einstein-Rosen and Schwarzschild black holes are different, physical realizations of general relativity. Yet for distant observers, both solutions are indistinguishable. We show that timelike geodesics in the field of a wormhole are complete because the expansion scalar in the Raychaudhuri equation has a discontinuity at the horizon, and because the Einstein-Rosen bridge is represented by the Kruskal diagram with Rindler's elliptic identification of the two antipodal future event horizons. These results suggest that observed astrophysical black holes may be Einstein-Rosen bridges, each with a new universe inside that formed simultaneously with the black hole. Accordingly, our own Universe may be the interior of a black hole existing inside another universe.

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