eps sci Lecture 3- Planetary Interiors

Ordinary matter

Composed of protons, neutrons, and electrons, defining atomic properties.

Protons

Particles that carry a positive charge in an atom.

Neutrons

Neutral particles in the nucleus of an atom that contribute to its atomic structure.

Electrons

Negatively charged particles that orbit the nucleus of an atom and define its chemical properties.

Phases of ordinary matter

Solid, liquid, gas, and plasma, each characterized by temperature and pressure conditions.

Density

Mass per unit volume, influencing how materials behave under pressure.

Temperature

The measure of average kinetic energy of particles, affecting matter's state.

Pressure

The force exerted per unit area, significant in understanding planetary interiors.

Outer core

The molten layer of Earth that generates its magnetic field through conductive material movement.

Inner core

The solid, primarily iron and nickel center of the Earth, under extreme conditions.

Mantle

The semi-solid, convective layer of the Earth above the outer core, essential for tectonic activity.

Crust

The outermost layer of the Earth, consisting of continental and oceanic plates.

Nuclear fusion

The process where lighter atomic nuclei combine to form heavier ones, releasing energy.

Supernova explosions

Catastrophic events occurring when a star exhausts its nuclear fuel, scattering elements into space.

Radiometric dating

A technique to determine the age of rocks and meteorites by measuring the decay of radioactive isotopes.

Chemical condensation sequence

The predicted order in which different compounds can condense as the solar nebula cools.

Differentiation

The process by which a planet's interior heats up and separates into distinct layers.

Cooling and evolution

The processes that planets undergo after formation, shaping their geological features.

Planetary composition

The materials that make up a planet, influenced by its formation and location in the solar system.

Frost line

The boundary in the solar nebula where hydrogen compounds condense into solid form.

Gravity

The force that influences the contraction and formation of celestial bodies in the solar nebula.

Accretion phase

The phase involving the growth of protoplanets through the collision and sticking of planetesimals.

Isotopes

Variants of elements that have the same number of protons but different numbers of neutrons.

Strong nuclear force

The force that holds protons and neutrons together in an atomic nucleus.