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Spacetime That Remembers A localized shear-front propagates across a deformable spacetime fabric. While the front passes, the fabric undergoes transient slip and shear. After it passes, a saturating memory field permanently modifies the weave, producing a non-reversible displacement. Particle constellations attached to the fabric settle into persistently shifted positions,... show more

Mathelirium

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58,446 次观看 • 5 个月前 •via X (Twitter)

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A shear-front crosses the frabric and Spacetime remembers. If you want the Python script to play with...subscribe and I will share.

A shear-front crosses the frabric and Spacetime remembers. If you want the Python script to play with...subscribe and I will share.

Mathelirium

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What Happens When a Black Hole Does More Than Fall? In General Relativity, a rotating Black Hole is described by the Kerr Metric. Its spin does something strange to spacetime... it drags the geometry around with it. The horizon sits at r₊ = M + √(M² - a²) but outside it there is another surface, the Ergosphere, r_E(θ) = M + √(M² - a²cos²θ) Inside that region, Spacetime is being swept around so strongly that remaining still is no longer possible. Every particle, every light thread, every local observer is forced to rotate with the geometry. For this scene, the C-metric acceleration remains alive in the background and the Black Hole still moves through the fabric, pulled along an axial defect. But the main event is Kerr frame dragging. The fabric twists. The Ergosphere breathes. Light paths shear into spirals. Particles that try to cross the region get carried around before falling inward. #GeneralRelativity #BlackHole #KerrMetric #FrameDragging #Ergosphere #Spacetime #EinsteinEquations #Astrophysics #Physics

What Happens When a Black Hole Does More Than Fall? In General Relativity, a rotating Black Hole is described by the Kerr Metric. Its spin does something strange to spacetime... it drags the geometry around with it. The horizon sits at r₊ = M + √(M² - a²) but outside it there is another surface, the Ergosphere, r_E(θ) = M + √(M² - a²cos²θ) Inside that region, Spacetime is being swept around so strongly that remaining still is no longer possible. Every particle, every light thread, every local observer is forced to rotate with the geometry. For this scene, the C-metric acceleration remains alive in the background and the Black Hole still moves through the fabric, pulled along an axial defect. But the main event is Kerr frame dragging. The fabric twists. The Ergosphere breathes. Light paths shear into spirals. Particles that try to cross the region get carried around before falling inward. #GeneralRelativity #BlackHole #KerrMetric #FrameDragging #Ergosphere #Spacetime #EinsteinEquations #Astrophysics #Physics

Mathelirium

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Two spinning Black Holes spiral through a warped Spacetime fabric, dragging it into twisting wells before merging into a single ringing remnant.

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Mathelirium

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When Light Becomes Heavy Enough to Trap Itself Can light collapse into a black hole? In General Relativity, light is not weightless in the geometric sense. It has energy, it carries momentum, and energy curves Spacetime. A Vaidya-type collapse describes a mass that grows because radiation is falling inward. The mathematics is the same brutal idea behind Einstein’s equation Gᵤᵥ = 8πTᵤᵥ If the stress-energy Tᵤᵥ is made from radiation, then light itself becomes a source of curvature. As more radiation falls inward, the mass aspect grows, the Spacetime fabric tightens, and a clean black horizon appears where escaping paths begin to fail. #GeneralRelativity #EinsteinEquations #BlackHole #Spacetime #Astrophysics #TheoreticalPhysics #Light #Mathematics #Science

When Light Becomes Heavy Enough to Trap Itself Can light collapse into a black hole? In General Relativity, light is not weightless in the geometric sense. It has energy, it carries momentum, and energy curves Spacetime. A Vaidya-type collapse describes a mass that grows because radiation is falling inward. The mathematics is the same brutal idea behind Einstein’s equation Gᵤᵥ = 8πTᵤᵥ If the stress-energy Tᵤᵥ is made from radiation, then light itself becomes a source of curvature. As more radiation falls inward, the mass aspect grows, the Spacetime fabric tightens, and a clean black horizon appears where escaping paths begin to fail. #GeneralRelativity #EinsteinEquations #BlackHole #Spacetime #Astrophysics #TheoreticalPhysics #Light #Mathematics #Science

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A coherent state wave packet oscillates in a 1D harmonic trap. - |ψ|² determines helix radius. - Phase determines helix twist. - The fabric deforms under the packet's pressure and current.

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With social fabric tearing on every front, Russians continue their collective descent into madness while queing for petrol. Never with a thought of merely remedying the situation by removing their army from Ukraine, they sacrifice their economy, society and eventually country to maintain the war.

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Can Spacetime Move Faster Than Light? In 1994, Miguel Alcubierre proposed a strange solution to Einstein’s field equations: A Spacetime geometry where a compact region could be transported without the object inside locally breaking the speed of light. The idea is not that a ship accelerates through space faster than light. The local interior remains comparatively calm. The violent part is the surrounding geometry. Space contracts in front of the bubble, expands behind it, and forms a moving transport shell that carries the interior region forward. A simplified form of the Alcubierre metric is ds² = −dt² + [dx − vₛ f(rₛ)dt]² + dy² + dz² where f(rₛ) shapes the warp bubble and vₛ describes the motion of its centre. The physics is still highly speculative, especially because the original construction requires exotic stress-energy, but the mathematical idea is powerful. #GeneralRelativity #AlcubierreDrive #WarpDrive #Spacetime #EinsteinEquations #Relativity #Physics #Astrophysics #Cosmology

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Mathelirium

198,553 次观看 • 5 个月前

In 1996, James Sethian showed something almost unfair...you can find shortest routes through a messy world by letting a wave expand once...no trial paths, no search beams, just one growing front. Here’s how: we solve for an arrival-time field T(x,y) so that T literally means how long the wave needs to reach this point. The rule is ||∇ T|| = 1/F, where the medium is fast (F large) the front sprints, where it’s slow it trudges, and obstacles are speed ≈ 0, so the front wraps around them because that’s the only way forward. Then comes the satisfying part: once T exists, a path doesn’t need to search at all...drop a bead anywhere and let it follow ẋ ∝ -∇ T, it slides downhill on the time landscape and traces a globally fastest route back to the source. This “wave = optimal control” viewpoint is exactly what Tsitsiklis (1995) made precise from the Hamilton-Jacobi side...compute the value/arrival-time function and the optimal trajectories fall out from it. #FastMarching #EikonalEquation

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Mathelirium

766,230 次观看 • 7 个月前