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Are there reliable raytraycing results showing the effect on light rays from far distant light emitters observed by (far distant) observers?

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- Thread starter tom.stoer
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In summary: Assuming I'm right in thinking that ray tracing is just null geodesics, the static schwarzschild should be the same as oppenheimer-snyder if you make sure light only passes in the external part of the metric, as the metric is the same.Yes--in a realistic simulation of what might be seen through a telescope.

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Are there reliable raytraycing results showing the effect on light rays from far distant light emitters observed by (far distant) observers?

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no ideas?

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push

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Is this of any interest? Seahra, "An introduction to black holes," http://www.math.unb.ca/~seahra/resources/notes/black_holes.pdf Has a bunch of discussion of horizons in the Vaidya metric.

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Assuming I'm right in thinking that ray tracing is just null geodesics, the static schwarzschild should be the same as oppenheimer-snyder if you make sure light only passes in the external part of the metric, as the metric is the same.

I'm guessing this may not be particularly helpful, though.

I'm guessing this may not be particularly helpful, though.

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Yes, simulated images; likebcrowell said:Simulated images?

http://pasj.asj.or.jp/v57/n3/570315/node4.html

http://www.wissenschaft-online.de/astrowissen/downloads/talks/pdf/RelEmLines.pdf

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Yes.pervect said:Assuming I'm right in thinking that ray tracing is just null geodesics, the static schwarzschild should be the same as oppenheimer-snyder if you make sure light only passes in the external part of the metric, as the metric is the same.

The Schwarzschild portion is growing with t to smaller r(t), therefore the images of rays not crossing r(t) are rays like in Schwarzschild spacetime with smaller r(t) but constant mass M.

But what I am especially interested in is the image of rays

a) passing through the dust ball (assuming that the dust is transparent)

b) close to r(t) in the far future where r(t) → 2M asymptotically

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http://www.wissenschaft-online.de/astrowissen/downloads/talks/pdf/RelEmLines.pdf

"Black hole collapse - ray tracing" is a theoretical concept in astrophysics that involves using mathematical calculations and computer simulations to study the gravitational collapse of a black hole and the behavior of light rays in its vicinity.

Ray tracing involves tracing the paths of light rays as they pass through the warped space and time around a collapsing black hole. By analyzing the paths of these rays, scientists can gain insight into the behavior of matter and energy near the event horizon of a black hole.

Studying black hole collapse is important because it can help us understand some of the most extreme and mysterious phenomena in the universe. It can also provide valuable insights into the nature of gravity and the fundamental laws of physics.

Studying black hole collapse can have practical applications in fields such as astrophysics, cosmology, and space travel. It can also help us better understand and predict the behavior of black holes, which are crucial objects in the formation and evolution of galaxies.

While ray tracing is a powerful tool for studying black hole collapse, it has its limitations. For example, it cannot fully account for quantum effects near the event horizon, and it relies on simplifying assumptions that may not accurately reflect the complexities of the real universe.

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