Using Einstein field equation

kashiark
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Gµv + Λgµv = (8πG/c4)Tµv
I have several questions. what is the µv? when we use it today do we use the cosmological constant even though the universe isn't static or does it mean something different than einstein orignally thought? what are we measuring when we use this if theyre all constants?
 
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I don't know the alt code either, but here's a copy-paster: Λ (from Wikipedia :))

The mu and nu are tensor indices, indicating that G, g and T are two-tensors. If you don't know what they are you should first of all learn about them, because they are very important constituents of the language in which GR is formulated (I recommend Carroll's book), but for now you can consider G, g and T as 4 x 4 matrices and mu, nu as simply indices, for example G00 is the top left component, etc.

The cosmological constant was written off a long time ago, but recently interest in it has arisen again. It can quite nicely explain some of the "odd" observed properties, such as the acceleration of the expansion rate of the universe and the fact that there seems to be more energy content than we'd expect. This might get you started, more advanced questions I will leave to the cosmologists out here :)
 
OK, so this has bugged me for a while about the equivalence principle and the black hole information paradox. If black holes "evaporate" via Hawking radiation, then they cannot exist forever. So, from my external perspective, watching the person fall in, they slow down, freeze, and redshift to "nothing," but never cross the event horizon. Does the equivalence principle say my perspective is valid? If it does, is it possible that that person really never crossed the event horizon? The...
ASSUMPTIONS 1. Two identical clocks A and B in the same inertial frame are stationary relative to each other a fixed distance L apart. Time passes at the same rate for both. 2. Both clocks are able to send/receive light signals and to write/read the send/receive times into signals. 3. The speed of light is anisotropic. METHOD 1. At time t[A1] and time t[B1], clock A sends a light signal to clock B. The clock B time is unknown to A. 2. Clock B receives the signal from A at time t[B2] and...
From $$0 = \delta(g^{\alpha\mu}g_{\mu\nu}) = g^{\alpha\mu} \delta g_{\mu\nu} + g_{\mu\nu} \delta g^{\alpha\mu}$$ we have $$g^{\alpha\mu} \delta g_{\mu\nu} = -g_{\mu\nu} \delta g^{\alpha\mu} \,\, . $$ Multiply both sides by ##g_{\alpha\beta}## to get $$\delta g_{\beta\nu} = -g_{\alpha\beta} g_{\mu\nu} \delta g^{\alpha\mu} \qquad(*)$$ (This is Dirac's eq. (26.9) in "GTR".) On the other hand, the variation ##\delta g^{\alpha\mu} = \bar{g}^{\alpha\mu} - g^{\alpha\mu}## should be a tensor...
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