Formation of Our Solar System

Nebulas Interstellar cloud containing gases such as hydrogen and helium and dust particles like carbon and iron. Irregular shape

Solar Nebulas Gravity pulls matter together. Very small gravitational attraction. Pressure pushes particles apart. Low temperatures-slow movement

Solar Nebulas Form Two or more Nebulas collide Nearby star explodes adding matter Gravity overcomes pressure Nebula collapses inward Solar system is formed

Planetesimals Nebula collapse Temperature and gravity increase Nebula begins to rotate Rotating nebula flattens into a disk Debris stick together forming small solid regions measuring one km across

Planets Larger planetesimals gain more material due to larger gravity Terrestrial and gas planets form Low temperatures allow gas giants to grow Warmer temperatures close to the sun allow inner planets to be solid

Birth of a Star Center of a Nebula contains the most mass. Hydrogen fusion begins. Gasses stopped collapsing 10 million years to form our Solar System

Planetary Motion Rotation-spinning motion on the axis giving us night and day Revolution-one complete lap around the sun Period of Revolution is called a year 365.25

Kepler’s First Law of Motion Planets moved around the sun in an elliptical orbit. • • focus Semimajor axis Major axis

Kepler’s Second Law of Motion Planets move faster when closer to the sun. Velocity has to increase due to an increase of gravitational attraction

Kepler’s Third Law of Motion Compares a planets period of revolution to it’s semimajor axis. Can determine a planets distance from the sun. Formula-P2=a3 ; P=period of revolution a=semimajor axis

Newton and Gravity All objects have mass therefore gravitational attraction. The Moon is falling around the Earth.