Big Bang Theory

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Singularity Noun

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[sing-gyoo-lar-i-tee]

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Singularity

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The theoretical, extremely hot and dense point from which the universe is believed to have begun its expansion.

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Example: This diagram shows a singularity as an infinitely dense point at the center of a black hole, where the fabric of spacetime is stretched to its limit.

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Redshift Noun

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[red-shift]

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Redshift

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The stretching of light waves from distant, receding objects, which increases their wavelength toward the red end of the spectrum.

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Example: As the universe expands over time, the space between galaxies stretches, causing the wavelength of light traveling through it to stretch and become redder.

Front

Hubble's Law Noun

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[hub-buhlz law]

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Hubble's Law

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The scientific law stating that galaxies are receding from an observer at a rate proportional to their distance from the observer.

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Example: This diagram shows that galaxies are moving away from us, and the farther away a galaxy is, the faster it is moving, which is Hubble's Law.

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Cosmic Microwave Background Radiation Noun

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[koz-mik my-kroh-weiv bak-ground rey-dee-ey-shuhn]

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Cosmic Microwave Background Radiation

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The faint, uniform thermal radiation filling all of space, considered to be the remnant energy from the Big Bang.

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Example: This map shows the faint heat left over from the Big Bang, with tiny red (hotter) and blue (colder) spots that grew into galaxies.

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Nucleosynthesis Noun

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[noo-klee-oh-sin-thuh-sis]

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Nucleosynthesis

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The cosmic process of creating new atomic nuclei from pre-existing protons and neutrons during various astrophysical events.

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Example: This diagram shows how simple particles like protons and neutrons fused together in the early, cooling universe to create the nuclei of heavier elements like helium.

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Big Bang Nucleosynthesis Noun

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[big bang noo-klee-oh-sin-thuh-sis]

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Big Bang Nucleosynthesis

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The formation of the first light elements, primarily hydrogen and helium, during the first few minutes after the Big Bang.

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Example: In the early universe, light atomic nuclei like deuterium (D) collided and fused, forming heavier nuclei like helium-3 (³He) and releasing other particles.

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Stellar Nucleosynthesis Noun

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[stel-er noo-klee-oh-sin-thuh-sis]

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Stellar Nucleosynthesis

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The process by which elements are created within stars through nuclear fusion reactions in their cores, forming elements up to iron.

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Example: Inside stars, three smaller Helium-4 atoms fuse together under immense pressure, creating one larger Carbon-12 atom and releasing a large amount of energy.

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Supernova Noun

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[soo-per-noh-vuh]

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Supernova

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The massive explosion of a star at the end of its life cycle, resulting in the creation and dispersal of heavy elements.

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Example: This diagram shows that a supernova is a massive explosion that occurs at the end of a high-mass star's life, after it has become a red supergiant.

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Supernova Nucleosynthesis Noun

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[soo-per-noh-vuh noo-klee-oh-sin-thuh-sis]

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Supernova Nucleosynthesis

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The formation of heavy elements, particularly those heavier than iron, during the intense conditions of a supernova explosion.

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Example: This diagram shows the balance of forces in a stable star, with gravity pulling in and pressure from heat pushing out, a state before a supernova.

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Baryonic Matter Noun

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[bar-ee-on-ik mat-er]

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Baryonic Matter

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Ordinary matter composed of protons and neutrons, which constitutes most of the visible matter in the universe like stars and planets.

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Example: This diagram compares a galaxy in the early universe to one today, showing how their rotation speeds differ, a concept used as evidence for dark matter.