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Chapter 16: Problem 6

Why do thermonuclear reactions occur only in the Sun's core, not in its outer regions?

Short Answer

Expert verified
Thermonuclear reactions occur only in the Sun's core because the extreme temperature and high pressure in the core provide the necessary conditions for hydrogen nuclei to overcome their repulsion and fuse into helium. The outer regions of the Sun lack these extreme conditions, therefore, are incapable of supporting such reactions.

Step by step solution

01

Understanding Thermonuclear Reactions

Thermonuclear reactions are nuclear reactions that are produced by the collision of nuclei, often leading to the transformation of elements. The most common example is the Sun; it generates energy through the fusion of hydrogen atoms into helium. The reaction requires temperatures of millions of degrees, which provides the necessary energy for the hydrogen nuclei to overcome their natural repulsion and come together.
02

Identifying the Conditions in the Sun's Core

The Sun's core is extreme in its temperature and pressure. It's where these thermonuclear reactions occur because the core has sufficiently high temperatures (approximately 15 million degrees Celsius) and pressure for the nuclear fusion of hydrogen into helium to take place. This region is dense and extremely hot, providing the ideal condition for thermonuclear reactions.
03

Comparing the Core to the Outer Regions

In contrast, the Sun's outer layers, including its photosphere, chromosphere, and corona, do not have the same extreme conditions as the core. The temperatures in these layers are substantially lower (ranging from about 5500 degrees Celsius in the photosphere to a few million degrees in the corona). Moreover, the density and pressure in these outer regions are also significantly less than in the core, which means they can't support thermonuclear reactions.

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Most popular questions from this chapter

What is Kelvin-Helmholtz contraction? Why is it ruled out as a source of the present-day Sun's energy?

Explain how the magnetic-dynamo model accounts for the solar cycle.

Calculate the wavelengths at which the photosphere, chromosphere, and corona emit the most radiation. Explain how the results of your calculations suggest the best way to observe these regions of the solar atmosphere. (Hint: Treat each part of the atmosphere as a perfect blackbody. Assume average temperatures of \(50,000 \mathrm{~K}\) and \(1.5 \times 10^{6} \mathrm{~K}\) for the chromosphere and corona, respectively.)

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