Modern Physics

Gravitational Waves

Ripples in spacetime from accelerating masses — predicted by Einstein, detected by LIGO

Gravitational waves are ripples in spacetime curvature caused by accelerating masses (especially compact binary mergers). Predicted by Einstein (1916), detected directly in 2015 by LIGO from a binary black hole merger. Carry energy at speed c, can pass through matter (almost) without interaction. Opens "gravitational wave astronomy" — observe events invisible to electromagnetic telescopes.

  • PredictedEinstein, 1916 (general relativity)
  • First direct detectionLIGO, 14 September 2015 (GW150914)
  • Source GW150914Two black holes merging, 1.3 billion ly away
  • Distortion size10⁻²¹ × baseline (LIGO 4 km arms → ~10⁻¹⁸ m)
  • Speedc (speed of light); confirmed by GW170817
  • Nobel Prize 2017Weiss, Barish, Thorne for LIGO

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Gravitational waves basics

From general relativity, accelerating massive objects radiate gravitational waves — ripples in spacetime that propagate at c. The wave amplitude is described by "strain" h = ΔL/L (fractional length change).

For typical sources at cosmological distances, h ≈ 10⁻²¹ at Earth. Tiny — but detectable with extreme precision instruments.

How they're generated

Quadrupole formula (Einstein, 1916):

P = (G/5c⁵) · <d³Q/dt³>²

where Q is the mass quadrupole moment. Power scales as ~v⁶ for binary inspirals.

Compact binary inspiral — two compact objects orbiting close, eventually merging. Frequency grows as orbit shrinks; sound: "chirp."

Major detected events

EventDateSourceSignificance
GW15091414 Sep 20152 BHs (36 + 29 M_sun)First direct detection
GW17081717 Aug 20172 NS (1.46 + 1.27 M_sun)First multi-messenger; kilonova
GW19052121 May 2019Heavy BH merger (85 + 66 M_sun)Intermediate-mass BH
GW19042525 Apr 2019Heavy NS-NS
GW2001055 Jan 2020NS-BH

Hundreds of detections so far across LIGO/Virgo/KAGRA observation runs.

JavaScript — gravitational wave calculations

const G = 6.674e-11;
const c = 3e8;
const M_sun = 1.989e30;

// Chirp mass (from binary inspiral)
function chirpMass(m1, m2) {
  // M_chirp = (m1*m2)^(3/5) / (m1+m2)^(1/5)
  return Math.pow(m1*m2, 0.6) / Math.pow(m1+m2, 0.2);
}

// GW150914
console.log(`GW150914 chirp mass: ${(chirpMass(36 * M_sun, 29 * M_sun) / M_sun).toFixed(2)} M_sun`);
// ~28 M_sun

// Strain at Earth from binary inspiral
function strain(chirpMass_kg, distance_m, frequency_Hz) {
  // h ~ (G·M_chirp/c²)^(5/3) · ω^(2/3) / (c·d)
  // Approximate; full formula is more complex
  const omega = 2 * Math.PI * frequency_Hz;
  return Math.pow(G * chirpMass_kg / (c * c), 5/3) * Math.pow(omega, 2/3) / (c * distance_m);
}

// GW150914 at ~100 Hz, 1.3 billion ly
const ly = 9.461e15;  // m
const distance_GW150914 = 1.3e9 * ly;
const Mchirp_GW150914 = 28 * M_sun;
console.log(`GW150914 strain: ${strain(Mchirp_GW150914, distance_GW150914, 100).toExponential(2)}`);
// ~10⁻²¹

// LIGO arm length distortion
function ligoDistortion(strain, arm_length_km) {
  return strain * arm_length_km * 1000;  // in meters
}

console.log(`LIGO 4km, h=10⁻²¹: ${ligoDistortion(1e-21, 4).toExponential(2)} m`);
// ~4 × 10⁻¹⁸ m — smaller than proton

// Power radiated (rough)
function gwPower(orbitalFreq, M_chirp) {
  // For two equal masses in circular orbit
  const omega = 2 * Math.PI * orbitalFreq;
  return (32/5) * Math.pow(G, 7/3) * Math.pow(M_chirp, 10/3) * Math.pow(omega, 10/3) / Math.pow(c, 5);
}

// Earth-Sun system: extremely small (Hz ~ 10⁻⁷)
console.log(`Earth-Sun GW power: ${gwPower(3.17e-8, 1).toExponential(2)} W`);
// ~10⁻⁹⁰ W — laughably small

// Frequency at coalescence (final orbit before merge)
function isco_freq(M_total) {
  // ISCO orbital freq ~ c³/(6√6 · π · G · M)
  return Math.pow(c, 3) / (6 * Math.sqrt(6) * Math.PI * G * M_total);
}

// 30 solar mass BH: f ~ 73 Hz
console.log(`30 M_sun BH ISCO: ${isco_freq(30 * M_sun).toFixed(0)} Hz`);
// ~73 Hz

Where GWs matter

  • Astrophysics. Black hole and neutron star mergers; populations and rates.
  • Multi-messenger astronomy. GW + EM + neutrinos for richer event understanding.
  • Cosmology. Standard sirens (GW + EM) for Hubble constant; primordial GW for inflation.
  • Tests of GR. Strong-field tests; ringdown spectra match Kerr BHs.
  • Heavy element creation. NS mergers produce gold, platinum (kilonova).
  • Future missions. LISA (2030s), Cosmic Explorer, Einstein Telescope.
  • Pulsar timing. Long-wavelength GWs from supermassive BH binaries (NANOGrav).

Common mistakes

  • Confusing GWs with gravity waves (atmospheric). Different — atmospheric "gravity waves" are buoyancy oscillations in fluids. GWs in physics are spacetime ripples.
  • Believing GWs travel through matter unchanged. Mostly yes, but at extreme densities (neutron stars), some interaction.
  • Thinking GWs need a medium. They're spacetime distortions — no medium needed. Travel through vacuum at c.
  • Underestimating energy. GW150914 emitted ~3 solar masses of energy in fraction of a second — more power than rest of observable universe combined.
  • Forgetting all moving masses radiate. Earth-Sun system also emits GWs (negligibly small). Only compact, high-acceleration sources detectable.
  • Believing speed of GWs ≠ c. GW170817 confirmed speed = c to 10⁻¹⁵ precision.

Frequently asked questions

What are gravitational waves?

Spacetime distortions propagating at light speed. Like ripples in a pond, but in 4D spacetime. Caused by accelerating masses — orbiting bodies, mergers, supernovae. Strain h = ΔL/L is the relative distortion. Tiny — for typical sources, h ~ 10⁻²¹. Over 4 km LIGO arm, distortion is 10⁻¹⁸ m — smaller than atomic nucleus.

How does LIGO detect them?

Two L-shaped 4-km Michelson interferometers (Hanford, WA and Livingston, LA). Laser light splits at corner, reflects off mirrors at each arm's end, recombines. Gravitational wave passing through changes path lengths slightly differently — interference pattern shifts. Can detect 10⁻¹⁸ m displacement (10,000× smaller than proton). Two detectors needed for cross-correlation and to rule out local noise.

What are the sources?

Major sources detected — binary black hole mergers (most common), binary neutron star mergers (rarer, also produce EM signals), neutron star-BH mergers. Future targets — supernovae, primordial GWs from inflation (CMB B-mode polarization). Sources detected by GW peak frequency: f ~ 100 Hz means objects ~50 km in size.

What's a "chirp" signal?

As two black holes spiral together, frequency increases (from a few Hz to hundreds), amplitude grows. Sounds like a chirp — characteristic signal. After merger, "ringdown" — final BH oscillates briefly before settling. Frequency, amplitude, and chirp pattern reveal masses, spins, distance.

How was Einstein's prediction confirmed?

GW150914 (Sept 14, 2015) — first direct detection. Two BHs (~36 + 29 solar masses) merged to ~62 solar mass BH; ~3 solar masses converted to GWs in fraction of a second. Energy released: more than all stars in observable universe combined for that instant. Frequency ramp up matched general relativity exactly.

What did the 2017 neutron star merger reveal?

GW170817 (Aug 17, 2017) — two neutron stars merged, observed in both gravitational waves AND electromagnetic spectrum (gamma rays, optical, X-rays). Confirmed: GWs travel at c (within 10⁻¹⁵), kilonova explosion produces heavy elements (gold, platinum), short gamma-ray bursts come from such mergers. Multimessenger astronomy.

What's the future of GW astronomy?

LISA (space-based, 2030s) — 2.5 million km arms; sensitive to lower frequencies (supermassive BHs, white dwarfs). Pulsar timing arrays (NANOGrav) — detect long-wavelength GWs from supermassive BH binaries. Cosmic Explorer, Einstein Telescope — upgraded ground-based observatories. Routine GW detection now (~50/year).