1. Section 2: Solar Activity Preview • Key Ideas • Sunspots • The Sunspot Cycle • Solar Eruptions • Auroras • Maps in Action

2. Key Ideas • Explainhow 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.

3. Sunspots • sunspota dark area of the photosphere of the sun that is cooler than the surrounding areas and that has a strong magnetic field. • 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.

4. 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 of the sun that appear darker than their surrounding regions. • These, cooler, darker areas are called sunspots. • The rest of the photosphere has a grainy appearance called granulation.

5. 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. • 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 of more sunspots. • After the peak, the number of sunspots begins to decrease until it reaches a minimum.

6. Sunspots Click below to watch the Visual Concept.

7. Solar Eruptions • 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. • This cycle is characterized by increases and decreases in various types of solar activity, including solar eruptions. • Solar eruptions are events in which the sun lifts substantial material above the photosphere and emits atomic or subatomic particles.

8. Solar Eruptions, continued • Solar eruptions include prominences, solar flares, and coronal mass ejections. Prominences • prominencea loop of relatively cool, incandescent gas that extends above the photosphere. • Each solar prominence follows the curved magnetic field lines from a region of one magnetic polarity to a region of the opposite magnetic polarity.

9. Solar Eruptions, continued Solar Flares • solar flarean explosive release of energy that comes from the sun and that is associated with magnetic disturbances on the sun’s surface • Solar flares are the most violent of all solar disturbances. • Solar flares release the energy stored in the strong magnetic fields of sunspots. This release can lead to the formation of coronal loops. • Some particles from a solar flare escape into space. These particles increase the strength of the solar wind.

10. Solar Eruptions, continued Coronal Mass Ejections • coronal mass ejectioncoronal gas that is thrown into space from the sun • As gusts of particles strike Earth’s magnetosphere, or the space around Earth that contains a magnetic field, the particles can generate a sudden disturbance to Earth’s magnetic field, called a geomagnetic storm. • Geomagnetic storms have been known to interfere with radio communications, satellites, and even cause blackouts.

11. 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.