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Relativity Advanced Quiz
Covers: e-equals-mc2, general-relativity, black-holes, gravitational-waves, cosmological-relativity
A nuclear reactor converts uranium into lighter elements and releases enormous energy. Where does that energy come from?
The chemical bonds between uranium atoms are broken
The electrons in uranium atoms are accelerated to high speed
The fission products have less total mass than the original uranium — the "missing" mass has been converted to energy via E = mc²
The neutrons inside the uranium atoms release stored kinetic energy
Mass-energy equivalence means mass and energy are interchangeable. When uranium fissions, the resulting fragments plus released neutrons have slightly less total mass than the original nucleus. That mass deficit — typically about 0.1% of the original mass — appears as kinetic energy of the fragments and radiation. The energy is enormous because the conversion factor is c², roughly 9 × 10¹⁶ joules per kilogram. Chemical reactions rearrange electrons and convert a negligible fraction of mass; nuclear reactions rearrange nucleons and access energy six orders of magnitude deeper.
In general relativity, what is gravity?
A force transmitted by graviton particles between massive objects
An attractive force that acts instantaneously across distance
The result of massive objects emitting gravitational waves that push other objects
The curvature of spacetime caused by mass and energy — objects follow geodesics (straightest paths) through curved spacetime
Einstein's central insight is that gravity is not a force at all. Mass and energy curve the geometry of spacetime, and objects in freefall follow geodesics — the straightest possible paths through that curved geometry. An orbiting planet is not being "pulled" by the Sun. It is moving in a straight line through spacetime that the Sun's mass has curved into an orbit. Newton's gravitational force is the low-speed, weak-field approximation of this geometric reality. The curvature framework eliminates action-at-a-distance entirely: spacetime is curved locally by local mass-energy, and objects respond to their local geometry.
What is the event horizon of a black hole?
The physical surface of the collapsed star
The point where the gravitational force becomes infinite
A causal boundary — the set of points from which no signal, including light, can ever reach a distant observer
The region where Hawking radiation is emitted
The event horizon is not a physical surface, not the singularity, and not where gravity becomes infinite. It is a causal boundary: the set of spacetime points from which outward-directed light rays can never escape to distant observers. An astronaut crossing the event horizon of a sufficiently large black hole would notice nothing locally — spacetime is smooth there, tidal forces can be mild, and local physics is normal. But once past the horizon, every possible future trajectory leads further inward. The horizon is defined by its causal property: it is the point of no return for information, the boundary beyond which events are permanently disconnected from the external universe.
How does LIGO detect gravitational waves?
By measuring changes in the gravitational force on suspended test masses
By using laser interferometry to detect differential length changes in two perpendicular arms — a passing gravitational wave stretches one arm and compresses the other
By detecting the electromagnetic radiation produced when gravitational waves interact with matter
By measuring the time delay of radio signals bounced between two widely separated stations
LIGO splits a laser beam and sends the halves down two perpendicular 4-kilometer arms. The beams reflect off mirrors and recombine. When both arms are exactly the same length, the beams destructively interfere — no signal. A gravitational wave stretches space along one arm while compressing it along the other, creating a tiny path-length difference that shifts the interference pattern. The sensitivity required is extraordinary: LIGO detects length changes of 10⁻¹⁸ meters, one-thousandth the diameter of a proton. Two detectors separated by 3,000 km provide correlation to distinguish astrophysical signals from local noise — the same principle as requiring consensus across distributed witnesses.
Why can we not observe the entire universe?
Our telescopes are not powerful enough to see that far
Intergalactic dust blocks light from the most distant regions
The universe is only 13.8 billion years old, so light from more distant regions has not had time to reach us
Beyond the cosmic horizon, the expansion of space carries regions away faster than light can cross the intervening distance — those regions are permanently causally disconnected from us
The cosmic horizon exists because space itself is expanding. Beyond a certain distance, the rate of spatial expansion exceeds the speed of light. Light emitted from those regions will never reach us — not because it has not had enough time, but because the distance it must cross is growing faster than it can travel. This is a permanent partition, not a temporary one. No future technology, no amount of waiting, will ever bring those regions into causal contact with us. Option C captures part of the story (the observable universe is finite) but misses the crucial mechanism: it is not a time limitation but a causal disconnection caused by the expansion rate exceeding c.
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