How Fast Is It - 05 - General Relativity II - Effects (1080p)
Δημοσιεύτηκε στις 13 Δεκ 2015
Text at http://howfarawayisit.com/documents/
In
this segment of the “How Fast Is It” video book, we cover the effects
of general relativity and how they differ from what Newton’s gravity
predicts. Our first effect is the orbit of Mercury that precesses more
than Newtonian gravity predicts. To understand the non-Euclidian space
that Mercury orbits in, we introduce the Schwarzschild metric and
compare it to the Minkowski metric for flat space-time. We illustrate
the positive curvature around the Sun using concentric circles with
shrinking circumferences. We then show how this slight difference in
curvature produces additional movement in the precessing perihelion of
Mercury’s orbit that exactly fits the measured number. Our next effect
is the bending of light. We cover Arthur Eddington’s famous measurement
during a total eclipse of the Sun and show how the amount of starlight
bending matched Einstein’s calculations better than Newton’s. We extend
this bending effect to show how Einstein Rings and gravitational lensing
work. And we show how this effect tips over light cones and changes
world-lines. Our third effect is gravitational time dilation. We show
how it works and cover how our GPS uses it. We also cover the
Pound-Rebka experiment used the Mossbauer Effect to showed how this time
dilation impacts gravitational redshift. We also illustrate how this
effect resolves the Twin Paradox we introduced in the Special Relativity
segment. Our final implication involves frame-dragging. To understand
this effect, we introduce the Kerr Metric that covers rotating energy
densities that literally drag space along with them. We use Gravity
Probe B to illustrate how it works and how it is measured. We finish
with an in depth look at the black hole in the movie Interstellar.
In
this segment of the “How Fast Is It” video book, we cover the effects
of general relativity and how they differ from what Newton’s gravity
predicts. Our first effect is the orbit of Mercury that precesses more
than Newtonian gravity predicts. To understand the non-Euclidian space
that Mercury orbits in, we introduce the Schwarzschild metric and
compare it to the Minkowski metric for flat space-time. We illustrate
the positive curvature around the Sun using concentric circles with
shrinking circumferences. We then show how this slight difference in
curvature produces additional movement in the precessing perihelion of
Mercury’s orbit that exactly fits the measured number. Our next effect
is the bending of light. We cover Arthur Eddington’s famous measurement
during a total eclipse of the Sun and show how the amount of starlight
bending matched Einstein’s calculations better than Newton’s. We extend
this bending effect to show how Einstein Rings and gravitational lensing
work. And we show how this effect tips over light cones and changes
world-lines. Our third effect is gravitational time dilation. We show
how it works and cover how our GPS uses it. We also cover the
Pound-Rebka experiment used the Mossbauer Effect to showed how this time
dilation impacts gravitational redshift. We also illustrate how this
effect resolves the Twin Paradox we introduced in the Special Relativity
segment. Our final implication involves frame-dragging. To understand
this effect, we introduce the Kerr Metric that covers rotating energy
densities that literally drag space along with them. We use Gravity
Probe B to illustrate how it works and how it is measured. We finish
with an in depth look at the black hole in the movie Interstellar.
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