About This Chapter
The Sun and Energy - Chapter Summary and Learning Objectives
Use this chapter to study the sun's life cycle, from its origins as a cloud of gas and dust to the phases of gravitational contraction. Our instructors can show you how the energy generated from this process created enough heat for nuclear fusion to occur. You can also take a closer look at the structure of the sun and learn how its sunspot cycle affects Earth. Lessons in this chapter are designed to teach you about the following:
- Gravitational contraction
- The life cycle of the sun
- Sun structure
- Steps in nuclear fusion
- The ideal gas law
|Structure of the Sun||Explore the radiative and convective zones in the sun's inner layers. Study the temperature of its outer layers.|
|The Sun's Atmosphere||Identify characteristics of the sun's chromosphere and corona.|
|Stages of the Sun's Life Cycle||Learn how nuclear fusion transformed the sun from a nebula into a main sequence star. Chart the sun's eventual development into a red giant and white dwarf.|
|Sunspots & the Magnetic Cycle||Discover the length of the sunspot cycle. Learn how it affects our climate.|
|Nuclear Fusion & the Sun||Differentiate nuclear fission from nuclear fusion. Explore steps in the proton-proton chain reaction.|
|Generating Energy Through Gravitational Contraction||Relate gravitational contraction to the sun's history.|
|The Ideal Gas Law and the Gas Constant||Explain the connection between variables represented in the ideal gas equation.|
|Using the Ideal Gas Law: Calculate Pressure, Volume, Temperature or Quantity of a Gas||Practice using the ideal gas equation to solve for unknown variables, such as pressure, volume, moles or temperature.|
1. Structure of the Sun
Discover the layers of the sun, including the core, radiative zone, convective zone, photosphere, chromosphere, and corona. Find out which layers you can see from Earth. Investigate what sunspots and solar flares are.
2. The Sun: Atmosphere & Facts
This lesson will go over what the three layers of our sun's atmosphere are, the sun's surface temperature, chemical composition, radius, and distance from Earth.
3. Photosphere: Definition & Features
This lesson will go over the sun's photosphere (its visible 'surface'), including where light comes from, how hot it is, and what granules and supergranules are.
4. Chromosphere: Definition & Properties
This lesson will explore some of the interesting features of the second layer of the sun's atmosphere, the chromosphere, including spicules and its pinkish hue.
5. The Solar Corona & Solar Wind
This lesson will define the solar corona and go over how it's involved with the formation of the solar wind and why it's hotter than the photosphere despite being the outermost layer of the sun's atmosphere.
6. Solar Flares, Solar Prominences & Coronal Mass Ejections
This lesson will go over three events caused by magnetic interactions in our Sun. They are prominences, flares, and coronal mass ejections. We'll also touch base on how the latter two can affect life on Earth.
7. Helioseismology & the Heliosphere
This lesson will go over important terms beginning with helio-: heliosphere, heliopause, and helioseismology - what they are and what importance helioseismology plays in our understanding of the sun.
8. What Are Sunspots?
This lesson will describe for you what sunspots are, where they appear, what parts they have, and why they're dark. It also discusses what differential rotation and a sunspot cycle are.
9. Why Do Sunspots Occur?
This lesson will outline for you why sunspots occur in its photosphere as we go over the Zeeman effect, polarity, and how the sunspot cycle and solar cycle are linked.
10. The Babcock Model of the Sun's Magnetic Cycle
This lesson will cover a model called the Babcock model or Magnetic-Dynamo model, which helps to explain how many of the features of the solar and sunspot cycle occur.
11. Stages of the Sun's Life Cycle
Discover our Sun, the provider of energy for life on Earth. Learn how the Sun was born, how it lives as a main sequence star, how it will age into a red giant and how it will die as a white dwarf.
12. How Energy Moves Within the Sun
This lesson will describe how energy is carried from the inner reaches of the Sun, through the radiative zone, then the convective zone, and finally into space.
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Other chapters within the Astronomy 101: Intro to Astronomy course
- The History of Astronomy
- How Scientists Think and Work
- Matter in Astronomy
- Light in Astronomy
- Newton's Laws in Astronomy
- Momentum, Energy, Pressure, Temperature & Gas
- Rotational Motion in Physics
- Earth's Spheres and Astronomy
- Influences on Climate
- The Orbits of Celestial Bodies
- The Earth, Sky, and Moon
- The Moon: Formation & Phases
- The Atmosphere on Earth and Other Planets
- The Solar System: Layout, Formation & Dating
- Characteristics of Our Solar System's Planets
- Small Celestial Bodies & Satellites in Our Solar System
- Measurement of Star Qualities
- Star Types and Significance
- The Birth and Life of Stars
- Star Death and Stellar Remnants
- The Milky Way Galaxy
- Galaxies: Properties & Characteristics
- The Universe: Key Concepts & Theories
- Life in the Universe
- Celestial Navigation & Timekeeping
- Relativity in Time and Space