OBJ: SWBAT identify parts of the sun and their characteristics

1. OBJ: SWBAT identify parts of the sun and their characteristics Drill: The sun contains approximately how much of the material within the solar system?

4. Chapter 29 Section 1 Structure of the Sun The Sun’s Energy, continued Nuclear Fusion • nuclear fusion the process by which nuclei of small atoms combine to form a new, more massive nucleus; the process releases energy • Nuclear fusion occurs inside the sun. Nuclei of hydrogen atoms are the primary fuel for the sun’s fusion. • Nuclear fusion produces most of the suns’ energy and consists of three steps.

5. The Final Product • One of the final products of the fusion of hydrogen in the sun is always a helium nucleus. • The helium nucleus has about 0.7% less mass than the hydrogen nuclei that combined to form it do. The lost mass is converted into energy during the series of fusion reactions that forms helium. • The energy released during the three steps of nuclear fusion causes the sun to shine and gives the sun its high temperature.

7. Chapter 29 Section 1 Structure of the Sun The Sun’s Interior The Core • Careful studies of motions on the sun’s surface have supplied more detail about what is happening inside the sun. The parts of the sun include the core, the radiative zone, and the convective zone. • At the center of the sun is the core. The core makes up 25% of the sun’s total diameter of 1,390,000 km. The temperature of the core is about 15,000,000 kmºC. • The core is made up entirely of ionized gas, and is 10 times as dense as iron.

9. Chapter 29 The Radiative Zone radiative zone the zone of the sun’s interior that is between the core and the convective zone and in which energy moves by radiation • The radiative zone of the sun surrounds the core. • The temperature of the radiative zone ranges from about 2,000,000ºC to 7,000,000 ºC . • In the radiative zone, energy moves outward in the form of electromagnetic waves, or radiation.

11. Chapter 29 Section 1 Structure of the Sun The Convective Zone Convective zone the region of the sun’s interior that is between the radiative zone and the photosphere and in which energy is carried upward by convection • The convective zone surrounds the radiative zone. The temperature of the convective zone is about 2,000,000ºC. • Convection is the transfer of energy by moving matter.

13. Chapter 29 Section 1 Structure of the Sun The Sun’s Interior, continued The diagram below shows the layers of the sun.

14. Chapter 29 Section 1 Structure of the Sun The Sun’s Atmosphere • The sun’s atmosphere surrounds the convective zone of the sun’s core. • Because the sun is made of gases, the term atmosphere refers to the uppermost region of solar gases. • The sun’s atmosphere has three layers: the photosphere, the chromosphere, and the corona.

15. Chapter 29 Section 1 Structure of the Sun The Photosphere photosphere the visible surface of the sun • Photosphere means “sphere of light.” The photosphere of the sun is the innermost layer of the sun’s atmosphere. • The photosphere is made of gases that have risen from the convective zone. The temperature in the photosphere is about 6,000ºC. • Much of the energy given off from the photosphere is in the form of visible light.

16. Chapter 29 Section 1 Structure of the Sun Reading Check What layers make up the sun’s atmosphere? The sun’s atmosphere consists of the photosphere, the chromosphere, and the corona.

17. Chapter 29 Section 1 Structure of the Sun The Chromosphere chromosphere the thin layer of the sun that is just above the photosphere and that glows a reddish color during eclipses • The chromosphere lies just above the photosphere. The chromosphere’s temperature ranges from 4,000°C to 50,000 °C. • The gases of the chromosphere move away from the photosphere, forming narrow jets of hot gas that shoot outward and then fade away within a few minutes.

18. Chapter 29 Section 1 Structure of the Sun The Sun’s Outer Parts corona the outermost layer of the sun’s atmosphere • The corona is a huge region of gas that has a temperature above 1,000,000ºC. • As the corona expands, electrons and electrically charged particles called ions stream out into space. • These particles make up solar wind, which flows outward from the sun to the rest of the solar system.

19. Chapter 29 Section 1 Structure of the Sun The Sun’s Atmosphere

21. Your Mission: Make a graphic organizer showing the layers of the sun and it’s atmosphere. Be sure to include:- Layer name-TemperatureImportant features ex) fusion

22. Identify the sun Layers!!

23. Chapter 29 Section 2 Solar Activity Objectives • Explain how sunspots are related to powerful magnetic fields on the sun. • Compare prominences, solar flares, and coronal mass ejections. • Describe how the solar wind can cause auroras on Earth.

24. Section 2 Solar Activity Chapter 29 Sunspots sunspot a dark area of the photosphere of the sun that is cooler than the surrounding areas and that has a strong magnetic field.

25. Sunspots • The movements of gases within the sun’s convective zone and the movements caused by the sun’s rotation produce magnetic fields. • These magnetic fields cause convection to slow in parts of the convective zone.

26. Chapter 29 Section 2 Solar Activity Sunspots • Slower convection causes a decrease in the amount of gas that is transferring energy from the core of the sun to these regions of the photosphere. • Because less energy is being transferred, these regions of the photosphere are considerably cooler than surrounding regions, and form areas fo the sun that appear darker than their surrounding regions. • These, cooler, darker areas are called sunspots.

28. Chapter 29 Section 2 Solar Activity The Sunspot Cycle • Observations of sunspots have shown that the sun rotates. • The numbers and positions of sunspots vary in a cycle that lasts about 11 years.

32. Sunspots initially appear in groups about midway between the sun’s equator and poles. The number of sunspots increases over the next few until it reaches a peak of 100 or more sunspots. • After the peak, the number of sunspots begins to decrease until it reaches a minimum.

33. Chapter 29 Section 2 Solar Activity Solar Ejections • Other solar activities are affected by the sunspot cycle, such as the solar-activity cycle. • The solar-activity cycle is caused by the changing solar magnetic field.

34. This cycle is characterized by increases and decreases in various types of solar activity, including solar ejections. • Solar ejections are events in which the sun emits atomic particles.

35. This cycle is characterized by increases and decreases in various types of solar activity, including solar ejections. • Solar ejections are events in which the sun emits atomic particles.

36. Solar ejections include prominences, solar flares, and coronal mass ejections.

37. Chapter 29 Section 2 Solar Activity Prominences prominence a loop of relatively cool, incandescent gas that extends above the photosphere.

38. Prominences are huge arches of glowing gases that follow the curved lines of the magnetic force from a region of one magnetic force to a region of the opposite magnetic polarity.

39. Chapter 29 Section 2 Solar Activity Solar Flares solar flare an explosive release of energy that comes from the sun and that is associated with magnetic disturbances on the sun’s surface

40. Chapter 29 Section 2 Solar Activity Coronal Mass Ejections coronal mass ejection a part of coronal gas that is thrown into space from the sun • Some of the particles from a solar flare escape into space, increasing the strength of the solar wind.

41. Particles also escape as coronal mass ejections. The particles in the ejection can cause disturbances to Earth’s magnetic field. • These disturbances have been known to interfere with radio communications, satellites, and even cause blackouts.

42. Chapter 29 Section 2 Solar Activity Solar Ejections, continued Reading Check How do coronal mass ejections affect communications on Earth? Coronal mass ejections generate sudden disturbances in Earth’s magnetic field. The high-energy particles that circulate during these storms can damage satellites, cause power blackouts, and interfere with radio communications.

43. Section 2 Solar Activity Chapter 29 Auroras aurora colored light produced by charged particles from the solar wind and from the magnetosphere that react with and excite the oxygen and nitrogen of Earth’s upper atmosphere; usually seen in the sky near Earth’s magnetic poles. • Auroras are the result of the interaction between the solar wind and Earth’s magnetosphere. • Auroras are usually seen close to Earth’s magnetic poles because electrically charged particles are guided toward earth’s magnetic poles by Earth’s magnetosphere.

44. Objective: SWBAT graph sunspot data IOT interpret and apply concepts of Solar Cycles • Drill: Blast from the past…. • What kind of clouds are dominating the weather this morning….. (hint: it was sprinkling)

45. Today you will graph sunspot data for a 30yr span. • Be sure to draw your scale appropriately IOT use as much of the graph paper as possible. • You will need a calculator

46. Objective: SWBAT graph sunspot data IOT interpret and apply concepts of Solar Cycles • Drill: Where does the energy come from that fuels the suns activity? Describe the process.

47. Anouncments… Quiz tomorrow!! Will cover sun layers, solar ejections, sunspots, and solar cycles. Today: Complete your sunspot cycle graph and questions. -You may want to extend your graph to answer the conclusion questions. - You will need to analyze the data provided IOT successfully answer the questions. (used a highlighter to highlight particular data of interest. This will help the data “stand out” - If you finish early, complete the Chapter 29 review # 1-39. You may omit #32. This will be due tomorrow morning.