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2m r in .NET framework
2m r QR Code 2d Barcode Decoder In .NET Using Barcode Control SDK for VS .NET Control to generate, create, read, scan barcode image in .NET framework applications. Generate Quick Response Code In VS .NET Using Barcode encoder for .NET framework Control to generate, create QR Code ISO/IEC18004 image in .NET framework applications. a2 r2
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Data Matrix ECC200 Generator In Java Using Barcode creator for Android Control to generate, create Data Matrix image in Android applications. Barcode Generation In Java Using Barcode drawer for Java Control to generate, create bar code image in Java applications. This horizon represents a boundary between the black hole and the outside world. It is analogous to the Schwarzschild horizon that we found in the case of a nonrotating black hole, and as we noted above, if you set a = 0 then you will get the familiar result r = 2m. Now, turning to the inner horizon represented by r = m m 2 a 2 , note that since it resides inside the outer horizon, it is inaccessible to an outside observer. Earlier we noted that in the Kerr geometry at rs = 2m, the time component of the metric vanishes, i.e., gtt = 0. The solution rs = 2m can be described as an outer in nite redshift surface that lies outside of the outer horizon r+ = m + m 2 a 2 . Particles and light can cross the in nite redshift surface in either direction. But think of the surface represented by the horizon r+ = m + m 2 a 2 as the actual black hole. It is the oneway membrane that represents the point of no return. If a particle or light beam passes it, escape is not possible. Interestingly, however, at = 0, the horizon and the surface of in nite redshift coincide, and so at these points if light or massive bodies cross, they cannot escape. The volume between these surfaces de ned by the static limit and the horizon, that is, the region where r+ < r < rs , is called the ergosphere. Inside the ergosphere one nds the framedragging effect: an object inside this region is dragged along regardless of its energy or state of motion. More formally we can say that inside the ergosphere, all timelike geodesics rotate with the mass that is the source of the gravitational eld. In between the two horizons where r < r < r + , r becomes a timelike coordinate. This is just like the Schwarzschild case. This means that if we were to nd ourselves in this region, no matter what we do, we would be pulled with inevitability to the Cauchy horizon r = r in the same way that we all march through life to the future. It is believed that the Kerr solution describes the geometry accurately up to the Cauchy horizon.

