By Thomas A. Moore

A normal Relativity Workbook is a textbook meant to help a one-semester undergraduate path on normal relativity. via its designated workbook-based layout, it allows scholars to improve a great mastery of either the physics and the helping tensor calculus via guiding them to paintings throughout the implications. the maths is brought steadily and in a totally actual context. every one bankruptcy, that's designed to correspond to 1 type consultation, comprises a quick assessment of the strategies with out obscuring derivations or information, by means of a chain of containers that advisor scholars during the means of operating issues out. This active-learning method allows scholars to improve a safer mastery of the cloth than extra conventional techniques. greater than 350 homework difficulties help additional studying.

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**Extra resources for A general relativity workbook**

**Example text**

Let us define coordinates so that v1 points in the +x direction. The particles then collide and form a single particle at rest with mass M= 2m. The total newtonian momentum of this system is clearly zero before and after the collision and so it is conserved in frame S. Now view this collision in a reference frame S´ that moves in the +x direction speed b = v. 30) while the other components of all three velocities remain zero. In frame S´, then, the total newtonian x-momentum is - 2mv/ (1 + v2) before the collision and –2mv after the collision, so newtonian momentum is not conserved in this frame.

Imagine that we turn the clock on its side so that the light flash moves parallel or anti-parallel to the clock’s motion. 11 still describes the relationship ∆t´ in the clock frame ∆t in the ground frame. 6 Imagine that a train is moving at a speed of 4/5. A passenger points a laser out the train window perpendicular to the tracks, and the laser emits a brief flash of light. What angle does the velocity of this light flash make with the tracks in the ground frame? 3 Four-Vectors Introduction Flat Spacetime • Review of Special Relativity • Four-Vectors • Index Notation Tensors • Arbitrary Coordinates • Tensor Equations • Maxwell’s Equations • Geodesics The Calculus of Curvature • The Absolute Gradient • Geodesic Deviation • The Riemann Tensor The Einstein Equation • The Stress-Energy Tensor • The Einstein Equation • Interpreting the Equation • The Schwarzschild Solution Cosmology • The Universe Observed • A Metric for the Cosmos • Evolution of the Universe • Cosmic Implications • The Early Universe • CMB Fluctuations & Inflation Gravitational Waves • Gauge Freedom • Detecting Gravitational Waves • Gravitational Wave Energy • Generating Gravitational Waves • Gravitational Wave Astronomy Schwarzschild Black Holes • The Schwarzschild Metric • Particle Orbits • Precession of the Perihelion • Photon Orbits • Deflection of Light • Event Horizon • Alternative Coordinates • Black Hole Thermodynamics Spinning Black Holes • Gravitomagnetism • The Kerr Metric • Kerr Particle Orbits • Ergoregion and Horizon • Negative-Energy Orbits 26 3 Four-Vectors t Describing Motion in Terms of Proper Time .

A line (maybe a curve). An object’s speed at any given instant is the inverse slope of the curve representing its worldline on the diagram, evaluated at that instant. Any light emitted by a given event E will expand (as time passes) into a spherical surface centered on the event. The projection of this sphere on the xy plane is a circle whose radius expands with time. 3). We call this the event’s light cone. The light cone is important because the worldline of any particle traveling through E must lie within this light-cone (because no particle can travel faster than light), and all events that can be caused by E must lie within this cone.