1. The Solar System
Chapter 23, Section 1

3. The Planets: An Overview
Terrestrial Planet – any of the Earth-like planets: Mercury, Venus, Earth, and Mars
Jovian Planet – the Jupiter-like planets: Jupiter, Saturn, Uranus, and Neptune; these planets have relatively low densities and are huge gas giants
Size is the most obvious difference between the terrestrial and the Jovian planets
The diameter of the largest terrestrial planet, Earth, is only ¼ the diameter of the smallest Jovian planet, Neptune; it’s mass is only 1/17 that of Neptune
Density, chemical makeup, and rate of rotation are other ways in which the two groups of planets differ
The densities of the terrestrial planets average about 5 times that of water, while the Jovian planets only average about 1.5 times that of water

5. Planets Drawn to Scale

6. The Interiors of the Planets
The substances that make up the planets are divided into 3 groups: gases, rocks, and ices
Gases – Hydrogen and Helium (melting point = -273oC)
Rocks – Silicate minerals and metallic iron (melting point = 700oC)
Ices – Ammonia, methane, carbon dioxide, and water (melting point = 0oC)
Terrestrial planets contain mostly rock material, while the Jovian planets contain the gases and ices.

7. The Interiors of the Planets

8. The Atmospheres of the Planets
A planet’s ability to retain an atmosphere depends on its mass and size
Jovian planets have thick atmospheres of hydrogen, helium, methane, and ammonia, due to their high surface gravities and the ability to hold on to the light gases
Terrestrial planets have very small atmospheres in comparison, with the atmosphere making up only a small portion of the planet’s mass

9. The Atmospheres of the Planets

10. Formation of the Solar System – Nebular Theory
Nebula – a cloud of dust and gas in space
These thin gaseous clouds begin to rotate and contract, and then spin faster
According to the nebular theory, the sun and planets formed from a rotating disk of dust and gases
As the speed of rotation increased, the center of the disk began to flatten out
The matter became more concentrated in the center, eventually igniting a nuclear reaction (the sun)

11. Formation of the Solar System – Planetesimals
Planetesimals – small, irregularly shaped bodies; formed from the collision of matter in space
As the collisions continued, the planetesimals grew larger, and began exerting their own gravity
In the inner solar system, it was so hot that only the metals and silicate materials could form
In the outer solar system, it was cool enough for the planets to attract ice and gases to add to their mass

12. Formation of the Solar System – Nebular Theory

13. Assignment Read Chapter 23, Section 1 (pg. 644-648)
Do Section 23.1 Assessment #1-7 (pg. 648)