In relativity, the Ricci curvature, which determines the collision properties of geodesics, is determined by the congruence of parallel null geodesics once it starts decreasing, will reach zero in a finite time.
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These lightcone coordinates have the useful feature that outgoing null geodesics are given by U = \ text { constant }, while ingoing null geodesics are given by V = \ text { constant }.
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These lightcone coordinates have the useful feature that outgoing null geodesics are given by U = \ text { constant }, while ingoing null geodesics are given by V = \ text { constant }.
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It only guarantees that if one follows the time-like geodesics into the future, it is impossible for the boundary of the region they form to be generated by the null geodesics from the surface.
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That is, when we look at the stars and say " The light from that star which I am receiving is X years old ", we are looking down this line of sight : a null geodesic.
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This last equation signifies that the particle is moving along a timelike geodesic; massless particles like the photon instead follow null geodesics ( replace " 1 with zero on the right-hand side of the last equation ).
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In General Relativity, as Allen notes above, this happens automatically because gravity isn't really a force after all and everything travels along null geodesics .-- SCZenz 15 : 32, 13 September 2006 ( UTC)
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Geodesics for massless particles are called " null geodesics ", since they lie in a " light cone " or " null cone " of spacetime, while those for massive particles are called " non-null geodesics ".
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Geodesics for massless particles are called " null geodesics ", since they lie in a " light cone " or " null cone " of spacetime, while those for massive particles are called " non-null geodesics ".
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Note that the null geodesics are of course " geometrically straight "; in the figure, they appear to be spirals only because the coordinates are " rotating " in order to permit the dust particles to appear stationary.
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