====== 1. Particle Age ====== ===== - Event highlights ===== Particle Age Timeline
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The Big Bang

The singularity event marking the origin of space, time, energy and matter (STEM). The universe emerges as an unimaginably hot and dense "primeval fireball".

10-35 to 10-32 seconds

Cosmic Inflation

A brief, exponential expansion where the universe swells in size by a factor of roughly 1050. This process smoothed out initial irregularities.

10-43 to 10-10 seconds

Separation of Forces

As the universe cooled, the single unified "superforce" separated into the four fundamental forces (energies) of nature: gravity, the strong nuclear force, the weak nuclear force, and electromagnetism.

10-35 to 1 second

Particle Creation & Annihilation

Energy converted into matter via "pair production". Quarks and leptons (e.g., electrons) emerged. Matter and antimatter collided and annihilated, leaving a slight excess of ordinary matter.

3 minutes to 15 minutes

Primordial Nucleosynthesis

The universe cooled sufficiently (below 109 K) for protons and neutrons to fuse. This "Nuclear Epoch" produced the first atomic nuclei: heavy hydrogen (deuterium), helium, and trace amounts of lithium.

50,000 years

Matter Domination

The "crossover point" where the energy density of matter finally exceeded that of radiation (or energy). This marked the end of the "Radiation Era" and the beginning of the "Matter Era," setting the stage for structure formation.

300,000 to 380,000 years

Recombination & Decoupling

Electrons combined with nuclei to form neutral atoms (recombination). This neutralized the charged fog, allowing photons to travel freely (decoupling), observable today as the Cosmic Microwave Background (CMB).

===== - Event details ===== {{:courses:ast100:particle-age.webp?nolink|}} The saga of our cosmos began at "time zero" with the Big Bang—a singular event that marked the simultaneous birth of space, time, energy, and matter. Emerging from a state of unimaginable density, the universe was not a traditional explosion bursting into an empty void; rather, it was a sudden eruption of space itself. This "primeval fireball" was so incredibly hot and compact that the standard laws of physics we rely on today simply did not yet exist. Almost instantly, in the blink of an eye between $10^{-35}$ and $10^{-32}$ seconds, the infant universe experienced a period of breath-taking growth known as Cosmic Inflation. In this fleeting moment, the fabric of space stretched by a staggering factor, expanding exponentially. This rapid transformation was vital for the future of the cosmos, as it smoothed out the early chaos and ensured that energy was distributed evenly enough to eventually allow for a stable and balanced universe. As the intense heat of the beginning began to fade within the first fraction of a second, the fundamental rules of nature started to take shape through the Separation of Forces. Initially, all of nature’s energy was bound together in a single "superforce." However, as the temperature dropped, this unity shattered, and the forces began to act independently. Gravity was the first to break away, followed by the nuclear and electromagnetic forces, setting the stage for the physical interactions that govern the world around us today. During the first full second of existence, the universe functioned as a colossal, high-energy furnace where light was constantly transforming into substance. In this era of Particle Creation and Annihilation, energy was converted into the basic building blocks of matter, such as quarks and electrons. While matter and antimatter engaged in a violent struggle, destroying one another upon contact, a tiny, fortunate excess of ordinary matter survived the conflict. This small remnant became the raw material used to build every star, planet, and person in existence. By the time the universe was three minutes old, it entered a crucial phase of "cosmic cooking" called Primordial Nucleosynthesis. This process was initially held back by a "bottleneck" where the environment was still too intense for simple atoms to hold together. However, once the temperature dipped below one billion degrees, the first atomic nuclei—primarily hydrogen and helium—could finally form and remain stable. This assembly line lasted only about fifteen minutes before the universe cooled too much to create anything heavier, leaving behind a chemical signature of roughly 75% hydrogen and 25% helium that we still see in the stars today. Following this initial frenzy, the universe expanded in total darkness for many thousands of years until it reached a pivotal turning point known as Matter Domination. At this stage, roughly 50,000 years after the start, the influence of matter finally became stronger than the influence of radiation. This shift was a defining moment in cosmic history; it allowed gravity to finally begin pulling matter together into the first large-scale structures, creating the invisible scaffolding upon which the first galaxies would eventually grow. Finally, between 300,000 and 380,000 years after the Big Bang, the universe cooled enough for electrons to settle into orbits around nuclei, forming the very first neutral atoms. This event, known as Recombination, cleared away the "charged fog" of particles that had previously trapped light. For the first time, the universe became transparent, allowing light to travel freely across the vastness of space. Today, we can still detect this ancient light as the Cosmic Microwave Background—a fossilized afterglow that serves as the ultimate "baby picture" of our universe.