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Special relativity

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In short

Special relativity is Einstein's 1905 theory of how space, time, momentum and energy transform between inertial frames moving at constant relative velocity, built on just two postulates and valid for all speeds up to c. It replaced Galilean kinematics once the Michelson-Morley experiment showed no ether and no dependence of light speed on the observer's motion. B.Sc Modern Physics papers under UGC CBCS devote a full unit to it, and GATE/JAM/NET, JEST and TIFR papers ask numerical questions on time dilation, invariant mass and relativistic kinematics every year. It is applied knowledge for roles at the Department of Atomic Energy, BARC, RRCAT Indore, VECC Kolkata, IUCAA and ISRO - accelerators, nuclear reactions, GPS timing corrections and cosmic-ray detection all need it.

Explained

Inertial frames, Galilean failure and the two postulates

Lorentz transformation and its immediate consequences

Velocity addition, Doppler effect and aberration

Relativistic dynamics: momentum, mass and energy

Spacetime, intervals and four-vectors

Limits, scope and where relativity hands over

Key points

Formulas and examples

γ = 1/√(1 − v²/c²) = 1/√(1 − β²), β = v/c (dimensionless); c = 2.998 × 10⁸ m/s
Lorentz boost: x′ = γ(x − vt), t′ = γ(t − vx/c²), y′ = y, z′ = z (x in m, t in s, v in m/s)
Time dilation: Δt = γΔτ (Δτ = proper time in s) Length contraction: L = L₀/γ (L₀ = proper length in m)
Simultaneity shift: Δt′ = γ(Δt − vΔx/c²)
Velocity addition: u = (u′ + v)/(1 + u′v/c²) Transverse: u_y = u′_y/[γ(1 + u′_x v/c²)]
Momentum p = γm₀u (kg·m/s); Total energy E = γm₀c² (J or MeV); KE K = (γ − 1)m₀c²
E² = p²c² + m₀²c⁴; for photons E = pc = hν; v/c = pc/E
Doppler (approaching) ν = ν₀√[(1+β)/(1−β)]; (receding) ν = ν₀√[(1−β)/(1+β)]; transverse ν = ν₀/γ
Invariant interval Δs² = c²Δt² − Δx² − Δy² − Δz²; proper time dτ = dt/γ
Conversions: 1 u = 931.49 MeV/c²; electron m₀c² = 0.511 MeV; proton m₀c² = 938.3 MeV; 1 eV = 1.602 × 10⁻¹⁹ J

Example 1 - Time dilation and length contraction at 0.8c. A spaceship of proper length 100 m passes Earth at v = 0.8c. Find γ, its length as measured from Earth, and the time an Earth observer assigns to a 1-hour process on board.

Example 2 - Cosmic-ray muon reaching sea level. A muon (proper lifetime τ = 2.2 μs) is created 10 km up and travels at v = 0.995c. Does it reach the ground?

Example 3 - Kinetic energy and the classical error. An electron is accelerated to v = 0.9c. Find γ, K, total energy and momentum (m₀c² = 0.511 MeV).

Example 4 - Velocity addition. Two probes leave Earth in opposite directions, each at 0.75c as seen from Earth. What is their relative speed?

Example 5 - Mass defect and fusion energy. In deuterium-tritium fusion, ²H + ³H → ⁴He + n releases a mass defect of 0.018883 u. Find the energy per reaction and per gram of fuel mixture.

QuantityClassicalRelativisticReduces to classical when
Momentummvγm₀vγ → 1
Kinetic energy½mv²(γ−1)m₀c²expand to first order
Velocity additionu′ + v(u′+v)/(1+u′v/c²)u′v ≪ c²
Time between eventsabsoluteγ × proper timev ≪ c
Length of a rodabsoluteL₀/γv ≪ c
Massconstant minvariant m₀ (γm₀ in old convention)always for m₀
v/cγK/m₀c²% error if ½mv² used
0.11.0050.00500.75%
0.51.1550.15519%
0.92.2941.29469%
0.997.0896.08992%

Where it is used

Interview questions

Common mistakes

Related topics

Quantum mechanics basics · Atomic and molecular physics · Nuclear and particle physics · Classical mechanics and Lagrangian dynamics · Electromagnetic theory and Maxwell's equations · Astrophysics and cosmology

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