Chapter 24: Studying the Sun. 24.3: The Sun Textbook pages

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1 Chapter 24: Studying the Sun 24.3: The Sun Textbook pages

2 The sun is one of the 100 billion stars of the Milky Way galaxy. The sun has no characteristics to make it unique to the universe. It is an average star. It IS, however, Earth s primary source of energy.

3 The sun is also the only star whose surface we can study. Because of its brightness and radiation, it s not safe to study the sun directly.

4 One of the finest telescopes for observing the sun in the world is located at Kitt National Observatory in southern Arizona.

5 Solar Statistics The sun s diameter is equal to 109 Earth diameters, or 1.35 million kilometers. The sun s volume is 1.25 million times as great as Earth s.

6 Its mass is 332,000 times the mass of Earth. The sun s density is only one quarter that of earth s. 90% of the sun s surface is hydrogen.

7 Structure of the Sun We can divide the sun into four parts: The solar interior The visible surface (photosphere) The two atmospheric layers: The Chromosphere The Corona

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9 The Sun s Visible Skin: Photosphere What words can you think of that include photo? Write them in your notes These words all refer to what phenomenon? What does this tell you about the photosphere?

10 The photosphere radiates most of the light that we see. It is a layer of gas about 500 kilometers thick.

11 The photosphere is not smooth and uniform. It is covered with spots known as granules. Each granule is about the size of Texas. They rise and sink in the surface due to convection. Sun Spot Granules

12 The Red Layer: Chromosphere The chromosphere lies directly above the photosphere. It is a few thousand kilometers thick. The chromosphere can only be seen during an eclipse or with special instruments. During an eclipse it appears as a narrow, spiky red ring around the sun.

13 This image of the sun s chromosphere was taken by a special telescope camera. You can see the photosphere in its gaps.

14 Corona: The Sun s Crown The corona is the outermost layer of the sun s atmosphere. It rests on top of the chromosphere. Like the chromosphere, the corona can only be seen during a total solar eclipse or with special instruments which block light shining from the photosphere.

15 This is an exceptionally dramatic photo of the corona, taken during a total solar eclipse. The corona can extend millions of kilometers into space.

16 Aurora Borealis The corona is very weak, and its surface is easily broken. The streams of protons and electrons which break through its gravitational pull are called solar winds.

17 When solar winds reach earth, they are pulled to the poles by our electromagnetic field. This results in a display of aurora borealis, or Northern Lights. (Most solar wind particles escape into space and don t reach earth.)

18 Auroras occur only at the north and south poles.

19 All of these photos were taken in Northern Alaska.

20 The Active Sun The sun has a dynamic, active surface which changes constantly. The most noticeable features on the sun are the dark regions. Before the telescope, it was thought that these dark areas were mini-planets in front of the sun, NOT part of it.

21 In 1610, Galileo observed that not only were these dark regions part of the sun, but that they were moving across the surface. Galileo concluded was that the sun rotated, AND that not all parts of the sun rotate at the same time!

22 Sunspots Sunspots are regions on the photosphere which are about 1,500 C less than the surrounding surface.

23 Sunspots have a cycle of about 11 years. At its height, more than a hundred sunspots can be spotted at a time. Then their numbers decline until only a few or none are visible.

24 Prominences Prominences are ionized gases trapped by magnetic fields that extend from regions of intense solar activity.

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28 They last about an hour, and appear as a sudden brightening arc above sunspot clusters. Solar Flare The most explosive events associated with sunspots are solar flares.

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30 Solar flares release enormous amounts of energy, in the form of ultraviolet, radio, and X-ray radiation waves.

31 This stream of atomic particles is called The Solar Wind. About a day after a large burst of solar flares, the particles will reach earth. They are attracted and flow to the earth s magnetic poles.

32 The interaction of magnetic fields and solar winds is the aurora borealis.

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