Is There Life Out There? Our Solar System (and beyond) Draw a picture of what you think life would look like on another planet, if it existed. Describe why you drew that image.

 Liquid water  Habitable Zone Habitable Zone  What can effect HZ?  Star – size and temperature  Distance from star  Size of planet  Structure of planet  Presence of atmosphere  Other source of heat What is needed for life to exist?

 How did it form?  Basic facts  99.8% of mass  100x diameter of Earth  5,527 o C  92.1% H, 7.8% He  Plasma  Sun today Sun today Our Sun

 Core  Dense  Hydrogen fusion  Radiative (radiation) zone  Uses radiation  Energy moves slowly  Convection zone  Uses convection  Materials rise and sink due to density  Moves more quickly Inner Solar Structure

 Photosphere  Visible surface  Chromosphere  Red  High speed gas  Corona  Hot  Outermost layer  Seen during an eclipse Outer Solar Structure

 Sunspots  Dark  Cold  Solar flares  High energy  Explosive  Prominence  Loops/arches Surface Feature Basics

1.VideoVideo  Write down your observations  Why did that happen? 2.Correct solar structure worksheet 3.What is needed for life as we know it? 4.Describe 3 things that would effect where life could be found in a solar system. Daily Review #1

Sunspot Lab

 What is a magnetic field?  What causes a magnetic field?  On the Sun?  Effect of rotation  Different rotation rates  Magnetic field lines get wound up  Eventually snap  Causes a solar flare  Solar prominences  Follow magnetic field lines into space Sun’s Magnetic Field

 Solar Quiz – Get out a computer and log on to your account Daily Review #2

 Cooler than nearby areas  Appear in pairs  Intense magnetic field  Lines go out and in  Predictable cycle  11-years  Minimums  Last = 2008  Low # of prominences, flares and sunspots  Cooler climate on Earth  Next maximum = 2013 Sunspots

 Hot, high speed, plasma streams  Corona expanding  Coronal Mass Ejections (CME)  Massive eruption  Rearrangement of magnetic field lines  One hit on 10/15/13  Effects on Earth  Disrupt magnetic field shape  Danger to astronauts  Damage electronics  Aurora Solar Wind

 Borealis or Australis  Interaction of particles and magnetic field  Particles drawn to poles  Colors  Elements  Altitude  Constantly changing  Video Video Aurora

 Astronomical unit (AU)  Average distance from Sun to Earth  1 AU= 9.3 x 10 7 mi = 1.5 x 10 8 km  Calculate the AU distance between the Earth and the Moon, 0.38 million km Distances within our Solar System

 Origin of the Solar System Our Solar System formed from a giant, swirling cloud of gas & dust.  Depends on two principles of Physics:  Newton’s Law of Gravity- gravitational potential energy ! heat  Conservation of angular momentum - rotational motion is conserved Nebular Theory

 Nebula  Inner edges  Heavier elements  Hotter  Rocky planets  Outer edges  Cooler  Lighter elements  Gas planets  Nebula  planetesimals  protoplanets Forming the Solar System

 Asteroid belt  Smaller bodies  Irregularly shaped  Orbit, but may wobble  Effected by Jupiter  May leave and collide with planets  Evidence for formation from one nebula  Nearly circular orbits  Orbit in same direction  Orbits in same plane  Planets rotate in same direction (mostly) Formation – cont.