The Big Bang, Cosmic Evolution, and Beyond in 3D

Key milestones

1. Hot and denseThe first instant
   T > 10³² Kz → ∞

   All the matter and energy of the observable universe is packed into a tiny, unimaginably hot region.

2. Space stretchesFractions of a second
   T ~ 10²⁷ Kz ~ 10²⁸

   Space itself expands, carrying everything apart: there is no centre and no edge to fly out from.

3. CoolingSeconds to minutes
   T ~ 10¹⁰ K → 10⁹ Kz ~ 10⁹

   As space stretches, the radiation filling it loses energy and the universe cools from trillions of degrees.

In the 3D scene 4 pointers

• Primordial Singularity

  The infinitesimally small, hot, dense initial state containing all observable mass-energy.

• Spacetime Coordinate Metric

  The 3D coordinate fabric of space itself stretching outward uniformly without an edge.

• High-Energy Particle Plasma

  Relativistic leptons, quarks and photons cooling from trillions of degrees.

• Cosmic Shockwave Front

  Outward relativistic wave boundary propagating through expanding space.

Key milestones

1. Quantum jitter10⁻³⁶ seconds
   T ~ 10²⁸ KPlanck Era

   At the smallest scales, energy flickers randomly: tiny quantum ripples.

2. InflationUntil 10⁻³² seconds
   SupercooledScale a × 10²⁶

   Space balloons in size by at least 10²⁶ times in a split second, faster than light can cross it.

3. Frozen ripplesAfter inflation
   T ~ 10²⁷ KReheating

   The ripples are stretched to cosmic size and frozen in as slightly denser and thinner regions: the seeds of galaxies.

In the 3D scene 4 pointers

• Inflaton Scalar Field

  High-energy scalar field with negative pressure that drove exponential cosmic ballooning.

• Quantum Density Ripples

  Subatomic Planck-scale ripples stretched to cosmological light-year dimensions.

• Frozen Ripple Seeds

  Overdense and underdense density perturbations frozen into space as the seeds of galaxies.

• Reheating Thermal Burst

  Decay of the inflaton field releasing standard-model particles and initiating the hot Big Bang.

Key milestones

1. A soup of quarksUnder a millionth of a second
   T ~ 2 × 10¹² KHadron Epoch

   Quarks and gluons fill space in a hot soup.

2. Protons and neutronsAbout a millionth of a second
   T ~ 10¹² KNucleon Freeze-out

   As it cools, quarks bind in threes into protons and neutrons.

3. The first nuclei3 to 20 minutes
   T ~ 10⁹ KBBN Period

   Protons and neutrons fuse into helium nuclei, until expansion cools the universe too much: 75% hydrogen, 25% helium.

In the 3D scene 4 pointers

• Quarks (u, d)

  Fundamental color charges (RGB) in high-energy plasma.

• Gluon Flux Confinement

  Strong nuclear force snapping quarks in triplets into stable nucleons at T ~ 10¹² K.

• Protons & Neutrons

  Nucleons (protons uud, neutrons udd) freezing out in a 7:1 ratio.

• Helium-4 (Alpha) Nuclei

  Tightly bound nuclei containing two protons and two neutrons forming 25% of cosmic baryonic mass.

Key milestones

1. A glowing fogThe first 380,000 years
   T > 3,000 °Cz > 1,100

   Free electrons scatter light constantly, so the universe is a hot, opaque, glowing fog.

2. The fog clears380,000 years
   T ≈ 3,000 Kz ≈ 1,100

   At about 3,000 °C, electrons join nuclei to make atoms, and light streams free.

3. The afterglowStill seen today
   T = 2.725 Kz = 0

   That light, stretched into microwaves, still arrives from every direction with tiny hot and cold spots: the seeds of galaxies.

4. The Dark Ages0.4 to ~100 million years
   T ~ 60 Kz ≈ 100 → 20

   With no stars yet, the universe goes dark while gravity slowly gathers gas.

In the 3D scene 5 pointers

• Thomson Scattering Fog

  Free electrons scattering photons constantly, rendering the early universe completely opaque.

• Recombination Neutral Atoms

  At T ≈ 3,000 K, protons capture electrons into neutral hydrogen atoms, clearing the fog.

• Free-Streaming Photons

  Decoupled light rays suddenly streaming freely across 13.8 billion years to reach modern telescopes.

• Sound Horizon (BAO) Ring

  Frozen acoustic sound wave shell in the primordial baryon-photon fluid (~150 Mpc comoving radius).

• Cosmic Microwave Background (CMB)

  The all-sky thermal afterglow cooled by expansion to 2.725 K with 10⁻⁵ temperature ripples.

Key milestones

1. The cosmic webTens of millions of years
   T ~ 30 Kz ≈ 25

   Gas and dark matter gather into a web of filaments with knots where they cross.

2. Collapse~100 million years
   T ~ 1,000 Kz ≈ 20

   In the densest knots, gas collapses and heats up.

3. First light from stars100–200 million years
   T ~ 10⁸ K (cores)z ≈ 15

   Fusion ignites: massive, blue-hot stars light up the universe.

4. ReionisationUp to ~1 billion years
   Ionising UVz ≈ 12 → 6

   Their ultraviolet light blows bubbles of ionised gas that grow and merge.

In the 3D scene 4 pointers

• Dark Matter Filaments

  Pristine cold dark matter web channeling primordial gas into gravitational knot wells.

• Gravitational Collapse Knots

  Cooling molecular hydrogen gas clouds collapsing past the Jeans mass threshold.

• Population III Hypergiants

  Zero-metallicity monster stars (100–300 M☉) burning at >50,000 K with lifespans of ~3 million years.

• Strömgren UV Ionization Bubbles

  Expanding spheres of re-ionized hydrogen gas carved out by ultraviolet starlight.

Key milestones

1. Primordial black hole seeds700 million years
   T ~ 10⁷ Kz ≈ 7

   Massive clouds of primordial gas collapse directly into giant black hole seeds.

2. Blazing accretion disk1 billion years
   T ~ 10⁸ Kz ≈ 6

   Infalling gas forms a superheated disk spinning near the speed of light, shining brighter than 1,000 Milky Ways.

3. Relativistic jets1.5 billion years
   Relativistic Plasmaz ≈ 4

   Twisted magnetic fields launch colossal particle jets from the poles, blowing gas out of the host galaxy.

In the 3D scene 5 pointers

• Kerr Event Horizon

  The central spinning boundary from which not even light can escape.

• Einstein Photon Ring

  Luminous circular photon orbit created by extreme gravitational light deflection.

• Accretion Disk (Doppler Beaming)

  Superheated gas orbiting at near-light speed; approaching side is blueshifted and bright.

• Relativistic Collimated Jets

  Twin magnetic particle beams launched along rotational poles at >0.99c spanning galaxy clusters.

• Infalling Galactic Feeding Streams

  Primordial gas clouds spiraling into the central gravitational well.

Key milestones

1. Dark matter skeleton2 billion years
   T ~ 30 Kz ≈ 3

   Invisible dark matter forms an intricate cosmic scaffold under the pull of gravity.

2. Filaments and voids5 billion years
   T ~ 10 Kz ≈ 1.5

   Galaxies flow along dense cosmic highways, leaving voids hundreds of millions of light-years across.

3. Superclusters and great walls8 billion years to present
   T = 2.73 Kz ≈ 0.5

   Thousands of galaxies cluster into massive complexes like the Laniakea Supercluster, where our Milky Way resides.

In the 3D scene 4 pointers

• Dark Matter Filaments

  Invisible gravitational highways linking massive galaxy clusters across deep space.

• Supercluster Nodes

  Overdense intersections where thousands of galaxies gather (e.g. Laniakea, Coma).

• Cosmic Voids

  Immense underdense bubbles (100–300 million light-years across) devoid of major galaxies.

• Gravitational Drift Streams

  Galaxies and intergalactic gas slowly migrating toward major cluster attractors.

Key milestones

1. Small galaxiesFirst billion years
   T ~ 10⁴ Kz ≈ 5 → 3

   Many small, irregular galaxies form in the knots of the cosmic web.

2. MergersBillions of years
   T ~ 10⁴ Kz ≈ 2 → 1

   They collide and merge, building bigger galaxies with tidal streams.

3. A spinning diskAbout 10 billion years ago on
   Disk Equilibriumz ≈ 0

   Gas settles into a flat, rotating disk where spiral arms form new stars.

In the 3D scene 5 pointers

• Sagittarius A* & Galactic Bulge

  A 4.15-million-solar-mass supermassive black hole surrounded by an ancient golden stellar bar.

• OB Starburst Clusters

  Young, hot blue stars illuminating the leading edges of spiral density waves.

• H II Emission Nebulae

  Glowing pink ionized hydrogen star-forming nurseries (e.g. Orion, Carina).

• Interstellar Dust Extinction Lanes

  Silhouetted ribbons of cold molecular gas and carbon/silicate dust grains.

• Globular Cluster Halo

  Spherical swarm of ancient 13-billion-year-old stellar clusters orbiting the galaxy.

Key milestones

1. A massive starMillions of years
   Core T ~ 4 × 10⁷ KLocal Stellar

   A massive star fuses hydrogen into helium in its core.

2. Layers like an onionIts last million years
   Core T ~ 3 × 10⁹ KPre-Supernova

   Near its end it fuses heavier elements in layers: carbon, oxygen, silicon, and finally iron at the centre.

3. CollapseUnder a second
   Core T ~ 10¹¹ KMillisecond Core Collapse

   Iron cannot release energy by fusion; the core collapses catastrophically into a neutron star.

4. SupernovaWeeks of brightness
   T ~ 10⁹ KBlast Wave v ~ 10⁴ km/s

   The star explodes, scattering its elements, and making more, into space.

In the 3D scene 5 pointers

• Convective Red Supergiant Envelope

  Enormous boiling atmosphere expanding past the orbit of Jupiter.

• Concentric Onion Fusion Shells

  Concentric burning layers: Hydrogen, Helium, Carbon, Oxygen, Neon, Silicon, and Iron.

• Inert Iron Core

  Chandrasekhar-mass core unable to generate fusion energy, collapsing in milliseconds.

• Supernova Detonation Blast

  Neutrino-driven shockwave blasting elements into interstellar space at 10,000 km/s.

• Spinning Pulsar Remnant

  Ultra-dense neutron star spinning dozens of times per second with relativistic magnetic beams.

Key milestones

1. The death spiralFinal orbits
   T ~ 10⁹ KBinary Orbit

   Two city-sized neutron stars, each heavier than the Sun, whirl around each other hundreds of times per second.

2. The collisionMilliseconds
   T > 10¹¹ KRelativistic Clash

   They crash together in a cataclysm that ripples spacetime and unleashes a blinding beam of gamma rays.

3. Forging heavy elementsDays to weeks
   Radioactive Glowr-Process

   A cloud of radioactive neutron-rich matter expands, forging several Earth-masses of gold and platinum (the r-process).

In the 3D scene 4 pointers

• Binary Neutron Stars

  City-sized ultra-dense stellar remnants whirling around each other at hundreds of orbits per second.

• Gravitational Wave Spirals

  Quadrupole ripples warping spacetime and carrying orbital energy away at the speed of light.

• Relativistic Collision Detonation

  Violent merger releasing gamma-ray burst jets and crushing matter past nuclear density.

• r-Process Golden Fireball

  Radioactive cloud synthesizing Earth-masses of gold, platinum, and uranium.

Key milestones

1. A cold cloud4.6 billion years ago
   T ~ 10–20 Kt = -4.6 Ga

   A cloud of hydrogen, helium and dust drifts in the Milky Way.

2. A shock waveA nudge
   Shock FrontTriggered Collapse

   A shock, perhaps from a nearby supernova, squeezes part of the cloud.

3. Collapse and spinTens of thousands of years
   T ~ 100–300 Kt = -4.57 Ga

   Gravity pulls the cloud in; like a skater pulling in her arms, it spins faster.

4. A disk and a protostar~100,000 years
   Protostar T ~ 4,000 KProtoplanetary Disk

   The cloud flattens into a spinning disk with a hot protostar at its heart.

In the 3D scene 5 pointers

• Supernova Shock Front

  External compression wave from a nearby exploding star triggering molecular cloud collapse.

• Rotating Protoplanetary Disk

  Centrifugal forces flattening the spinning gas cloud into a Keplerian accretion disk.

• Nascent Protostar (Young Sun)

  Gravitational core growing in mass and heating up to become our Sun.

• Bipolar Herbig-Haro Jets

  Magnetic plasma outflows launched perpendicular to the disk to shed excess angular momentum.

• Planetesimal Ring Gaps

  Dark concentric circular lanes cleared out by infant giant planets (proto-Jupiter).

Key milestones

1. Accelerating expansionTens of billions of years
   T ~ 2.7 K → 1 Kz → -1

   Dark energy accelerates expansion: all galaxies outside our local group disappear beyond the cosmic event horizon.

2. The last stars fade1 to 100 trillion years
   T → near 0 KStelliferous Sunset

   Gas is exhausted, and the longest-lived red dwarfs cool into dark black dwarfs. The Stelliferous Era ends.

3. The Big Freeze & heat death10⁴⁰ to 10¹⁰⁰ years and beyond
   T ≈ 0 K (-273.15 °C)Heat Death

   Only black holes remain, slowly evaporating away via Hawking radiation until space is cold, calm, and empty.

In the 3D scene 4 pointers

• Cosmological Event Horizon

  The boundary beyond which accelerating spatial expansion prevents light from ever reaching us.

• Receding Redshifted Galaxies

  Distant galaxy clusters slipping beyond causal contact as dark energy dominates.

• Degenerate Stellar Embers

  Burned-out white dwarfs and red dwarfs slowly cooling into dark black dwarfs.

• Hawking Radiation Evaporation

  Faint quantum particle emission slowly radiating away black holes over 10¹⁰⁰ years.