Astrochemistry primarily focuses on understanding the chemical reactions and processes that occur in various cosmic environments.

The Big Bang is considered to be the initial event that led to the formation of the first complex molecules through nucleosynthesis.

Interstellar chemistry refers to the chemical reactions that take place within interstellar clouds, leading to the formation of various molecules and compounds.

Hydrogen (H2) is the most abundant molecule in the universe, accounting for approximately 75% of all matter.

Carbon is crucial in astrochemistry due to its ability to form various complex molecules, its role in the origin of life, and its presence in interstellar dust.

Formaldehyde (H2CO) is often referred to as 'interstellar formaldehyde' due to its widespread presence in interstellar clouds.

Grain-surface chemistry refers to the chemical reactions that occur on the surfaces of interstellar dust grains, leading to the formation of various molecules.

Hydrogen cyanide (HCN) is a crucial precursor to the formation of amino acids, which are the building blocks of proteins.

Cometary chemistry focuses on analyzing the chemical composition of comets, providing insights into the early solar system and the origin of organic molecules.

Diatomic carbon (C2) is responsible for the distinctive green color often observed in comets.

Cosmic rays, consisting of high-energy particles, are the primary source of energy driving chemical reactions in interstellar clouds.

The presence of water (H2O) in interstellar clouds is often inferred through the detection of its rotational transitions.

Stellar chemistry focuses on the chemical reactions and processes that take place within the atmospheres of stars.

Hydrogen cyanide (HCN) is a key molecule involved in the formation of carbon-based molecules in interstellar clouds.

Meteoritic chemistry involves analyzing the chemical composition of meteorites to gain insights into the early solar system and the origin of organic molecules.