Terrestrial Planets: Mercury and the Moon
Introduction to Terrestrial Planets
Class: AST101: The Sun and its Neighbours, Professor C. Barth Netterfield
Overview of the Solar System
Major terrestrial planets: Mercury, Venus, Earth, Mars
Key terminology:
Astronomical Unit (AU): Standard unit of measurement in astronomy, reflecting the average distance from the Earth to the Sun.
Ceres: Dwarf planet located in the asteroid belt.
Formation of Terrestrial Planets
Molecular Clouds
Gravity pulls a molecular cloud (gas and dust) together, collapsing it.
Conservation of momentum causes the cloud to spin faster, flattening orbits.
Results in a spinning disk of gas and dust.
Planetesimals Formation
Tiny objects stick together to form planetesimals, which are the seeds or cores of planets.
Frostline and Material Composition
Inside and Outside the Frostline
Frostline: Divides regions where different materials can form planetesimals.
Inside the Frostline:
0.2% Metals (Solid)
0.4% Rocks (Solid)
1.4% Hydrogen Compounds (Gas)
98% Helium and Hydrogen (Gas)
Outside the Frostline:
0.2% Metals (Solid)
0.4% Rocks (Solid)
1.4% Hydrogen Compounds (Solid Ice)
98% Helium and Hydrogen (Gas)
Characteristics of Terrestrial Planets
General Traits:
Small size
Rocky composition
Relatively thin or non-existent atmosphere
Few moons
Composed primarily of heavy elements (rock and metal)
Planets Included: Mercury, Venus, Earth, Mars, and Earth's Moon.
Crater Formation on Terrestrial Bodies
Characteristics of Craters
Present in various sizes and overlapping on Mercury and the Moon.
Created when a planetesimal strikes the surface at speeds of approximately 100,000 km/hr.
The collision vaporizes surface rock, leading to an explosion that forms a crater.
Implications of Crater Density
Heavy Bombardment: A time when planetesimals were abundant, causing numerous impacts.
Significant decrease in impacts post-heavy bombardment (~4 billion years ago).
Understanding Planet Interiors
Methods to Probe Interior Structures
Drilling: Impossible due to depth limitations (max depth ~12 km vs Earth's radius of 6371 km).
Seismology: Utilizes earthquake vibrations to understand planetary interiors.
P Waves: Compressional waves that can travel through solids and liquids.
S Waves: Shear waves that cannot travel through liquids, indicating liquid core presence.
Internal Composition of Planets
Layers defined by density: Low-density rock, medium-density rock, high-density iron and nickel core.
Differentiation: Process whereby lighter materials rise to the surface and heavier materials sink to the core.
Heat Sources in Planets
Why are Planet Interiors Hot?
Accretion: Generated heat during planet formation.
Differentiation: Significant in early formation.
Radioactive Decay: Currently the primary source of internal heat.
Cooling Processes in Planets
Methods of Cooling
Convection: Hot mantle rock rises, cooler rock sinks, transferring heat from the core.
Conduction: Slow heat transfer through the rigid crust.
Radiation: Infrared light escapes the surface, cooling the planet.
Influences of Planet Size
Small planets cool faster due to higher surface area-to-volume ratios.
Formula impact: As radius doubles, volume increases by 8 times while surface area increases by only 4 times.
Surface Changes on Moons and Planets
Cratered Surfaces
Areas of smooth surfaces (Mares) result from earlier molten lava flooding over cratered surfaces post-heavy bombardment.
Both Mercury and Earth's Moon have similar surface histories.
Recent Surface Changes
Exploration of other moons (e.g., Enceladus) to assess surface age and activity.
Conclusion
Terrestrial planets share similarities in composition and structure, with variations influenced by their history, formation processes, and proximity to the Sun.