1. Start of Class 1. Pick up your work from the front table. 2. Get a blank piece of paper and draw something like this 2/24/2016describe how the planets developed

2. Sunspot Lab 1. What are sunspots? How they form, how long they last, is there a cycle. 2. On your drawings, how many sunspots did you see? Was it what you would expect in a solar maximum period? 3. Do you think the sun would look the same after 10 minutes, What will change or not change 2/24/2016describe how the planets developed

3. Video Notes – The Sun How did early man use the sun? How did we determine the energy output of the sun? What do we do to determine the sun’s make up? What does it tell you about the sun’s core, the outer layers, the fusion process and a use for it? What does it tell you about sunspots, prominences and flares ? 2/24/2016describe how the planets developed

4. Warm Up Write out a chapter outline. Clue page 570 Essential Question: Explain how the sun converts matter into energy Exit Question: In your own words, write an explanation on how the sun converts matter. Homework: Chapter 28 vocabulary, term- define-fact, page 586 due Friday 9/5/14 2/24/2016describe how the planets developed

5. 2/24/2016describe how the planets developed Chapter 28.1 Objectives Explain how the sun converts matter into energy in its core Compare the Radiative and convection zones of the sun Describe the three layers of the sun’s atmosphere

6. 2/24/2016describe how the planets developed Chapter 28.1 Notes Until recently most people thought the sun energy was fire. We now use spectroscopic analysis of the sun’s rays Have studied the inner layers of the sun; the core, the inner zones and the atmosphere

7. Explain how the sun converts matter into energy in its core The core is 15,000,000C and is 10% of the sun’s diameter of 1,300,000 km Has 300,000 times our mass and therefore more gravity There is enough pressure in the core to strip electrons from atoms This creates plasma and allows nuclear fusion to take place 2/24/2016describe how the planets developed

8. Explain how the sun converts matter into energy in its core 1. Two protons collide and fuse 2. One changes into a neutron 3. Another proton collide and fuse with the neutron and proton 4. This collides with another nuclei of the same 5. Two protons thrown off 2/24/2016describe how the planets developed

9. Explain how the sun converts matter into energy in its core Einstein proposed that a small amount of matter can create a large amount of energy E=mc 2 is the theory of relativity that show how much energy is created from matter The sun coverts 600 million tons of Hydrogen a second 2/24/2016describe how the planets developed Page 571 for more information

10. 2/24/2016describe how the planets developed Compare the Radiative and convection zones of the sun The core 15,000,000C : energy is generated in the core Radiative zone surrounds core 2,500,000C : Energy transferred atom to atom, like a wave on the waters surface Convection zone 1,000,000C : energy is transferred in large circulation of plasma, colder at the sun’s surface and hotter as you near the radiative zone – page 574

11. 2/24/2016describe how the planets developed Describe the three layers of the sun’s atmosphere Upper three layers of sun after convection zone Photosphere or light – energy bubbles up here as light so we call it the surface, 6,000C The Chromosphere is a reddish zone that seems to form jets off the photosphere Corona is the outer layer that prevents energy loss

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13. 2/24/2016describe how the planets developed Chapter 28.2 Objectives Explain how sunspots are related to powerful magnetic fields on the sun. Compare prominences and solar flares. Describe how the solar wind can cause auroras on the earth.

14. Chapter 28.2 Notes Gravity and Fusion cause solar materials to constantly rise and fall Gas also moves because of the solar rotation The equator rotates in 25.3 days The poles in 33 days Average is 27 days 2/24/2016describe how the planets developed

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16. Explain how sunspots are related to powerful magnetic fields on the sun. The up and down movement of the gases cause strong magnetic fields These magnetic fields cause the convection currents to slow Less material is raised to the photosphere – cool spots form 3,000C The sunspot cycle is a 11 year period – most form at the equator – last low was 2008 2/24/2016describe how the planets developed

17. 2/24/2016describe how the planets developed Sunspots

18. 2/24/2016describe how the planets developed Compare prominences and solar flares. 1. The magnetic fields cause large clouds of hot gas to arch high above the sun’s surface 2. The arch follows the magnetic field lines; can last a few days to a year 3. Solar flares a violent eruptions of gas; can last several hours 4. Flares thrown into space; cause magnetic storms on earth that can effect radio communication

19. Describe how the solar wind can cause auroras on the earth. Caused by magnetic storms from the sun Charged particles move along earths magnetic fields and strike gases in the atmosphere They are 100km to 1,000km above the surface Sometimes called the northern or southern lights 2/24/2016describe how the planets developed

20. 2/24/2016describe how the planets developed Solar Wind Interaction with Magnetosphere

21. 2/24/2016describe how the planets developed Video Questions – The SunThe Sun What powers the sun and what is it made of? How is the solar system formed? Explain the suns magnetic field. Explain the current theory of the end of our solar system.

22. Chapter 28.3 Objectives Explain the Nebular theory of the origin of the solar system. Describe how the planets developed. Describe the formation of the land, the atmosphere, and the oceans of the earth. 2/24/2016describe how the planets developed

23. 2/24/2016describe how the planets developed Explain the Nebular theory of the origin of the solar system. 5 Billion years ago….. Explosion of nearby supernova caused nebula to condense and spin – SOLAR NEBULA PROTOPLANETS Planetesimals combined to form PROTOPLANETS – “pre- planets”

24. 2/24/2016describe how the planets developed Explain the Nebular theory of the origin of the solar system. Formation of the Sun & Planets Nebular Theory Solar Nebula Planetesimals  Protoplanets

25. 2/24/2016describe how the planets developed Describe how the planets developed. Formation of the Earth 3 Sources of Heat Primordial Heat Left over heat from formation of Earth Compression of outer layers Radioactive Material in Core The Solid Earth Core-Dense Core of Nickel & Iron Mantle Crust of less dense materials

26. 2/24/2016describe how the planets developed Describe the formation of the land, the atmosphere, and the oceans of the earth Hydrogen & Helium found in nebulae Lithium  Iron formed in core of stars from fusion Nickel  Plutonium formed during explosion of supernovae and re- condense in new nebula Is the Earth an “Original Planet?” Why?

27. 2/24/2016describe how the planets developed Describe the formation of the land, the atmosphere, and the oceans of the earth

28. 2/24/2016describe how the planets developed Describe the formation of the land, the atmosphere, and the oceans of the earth FIRST Original (FIRST) Atmosphere probably lost to solar winds Present Atmosphere results from Outgassing Hydrogen & Helium abundant in Solar Nebula – where did water come from? Volcanic eruptions released MASSIVE amounts of carbon dioxide & water

29. 2/24/2016describe how the planets developed Describe the formation of the land, the atmosphere, and the oceans of the earth Reducing  Oxidizing Atmosphere Sunlight caused Ammonia and water to form NITROGEN GAS Cyanobacteria & photosynthetic plants converted nitrogen to energy making OXYGEN WASTE PRODUCT Oxygen reacted with sunlight to form OZONE – PROTECTIVE LAYER With more ozone, life was able to thrive With more ozone, life was able to thrive

30. 2/24/2016describe how the planets developed Describe the formation of the land, the atmosphere, and the oceans of the earth 3 to 3.5 BILLION years ago, the Earth cooled enough to allow water to form from steam Rain fell and oceans formed in lower areas Today’s atmosphere has been constant for last 1.5 Billion years