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Chapter 15--Our Sun - Geological Sciences

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COMMON MISCONCEPTIONS<br />

The <strong>Sun</strong> Is Not on Fire<br />

fission<br />

fusion<br />

We are accustomed to saying that the <strong>Sun</strong> is “burning,”<br />

a way of speaking that conjures up images of a giant bonfire<br />

in the sky. However, the <strong>Sun</strong> does not burn in the<br />

same sense as a fire burns on Earth. Fires on Earth generate<br />

light through chemical changes that consume oxygen<br />

and produce a flame. The glow of the <strong>Sun</strong> has more<br />

in common with the glowing embers left over after the<br />

flames have burned out. Much like hot embers, the <strong>Sun</strong>’s<br />

surface shines with the visible thermal radiation produced<br />

by any object that is sufficiently hot [Section 6.4].<br />

However, hot embers quickly stop glowing as they<br />

cool, while the <strong>Sun</strong> keeps shining because its surface is<br />

kept hot by the energy rising from the <strong>Sun</strong>’s core. Because<br />

this energy is generated by nuclear fusion, we<br />

sometimes say that it is the result of “nuclear burning”—<br />

a term that suggests nuclear changes in much the same<br />

way that “chemical burning” suggests chemical changes.<br />

Nevertheless, while it is reasonable to say that the <strong>Sun</strong><br />

undergoes nuclear burning in its core, it is not accurate<br />

to speak of any kind of burning on the <strong>Sun</strong>’s surface,<br />

where light is produced primarily by thermal radiation.<br />

No real spacecraft could survive, but your imaginary<br />

one keeps plunging straight down to the solar core.There<br />

you finally find the source of the <strong>Sun</strong>’s energy: nuclear fusion<br />

transforming hydrogen into helium. At the <strong>Sun</strong>’s center,<br />

the temperature is about <strong>15</strong> million K, the density is more<br />

than 100 times that of water, and the pressure is 200 billion<br />

times that on the surface of Earth. The energy produced<br />

in the core today will take about a million years to<br />

reach the surface.<br />

With your journey complete, it’s time to turn around<br />

and head back home. We’ll continue this chapter by studying<br />

fusion in the solar core and then tracing the flow of the<br />

energy generated by fusion as it moves outward through<br />

the <strong>Sun</strong>.<br />

<strong>15</strong>.3 The Cosmic Crucible<br />

The prospect of turning common metals like lead into<br />

gold enthralled those who pursued the medieval practice<br />

of alchemy. Sometimes they tried primitive scientific approaches,<br />

such as melting various ores together in a vessel<br />

called a crucible. Other times they tried magic. Their getrich-quick<br />

schemes never managed to work. Today we<br />

know that there is no easy way to turn other elements into<br />

gold, but it is possible to transmute one element or isotope<br />

into another.<br />

If a nucleus gains or loses protons, its atomic number<br />

changes and it becomes a different element. If it gains or<br />

Figure <strong>15</strong>.5 Nuclear fission splits a nucleus into smaller nuclei<br />

(not usually of equal size), while nuclear fusion combines smaller<br />

nuclei into a larger nucleus.<br />

loses neutrons, its atomic mass changes and it becomes a<br />

different isotope [Section 4.3].The process of splitting a nucleus<br />

into two smaller nuclei is called nuclear fission.The<br />

process of combining nuclei to make a nucleus with a greater<br />

number of protons or neutrons is called nuclear fusion<br />

(Figure <strong>15</strong>.5). Human-built nuclear power plants rely<br />

on nuclear fission of uranium or plutonium. The nuclear<br />

power plant at the center of the <strong>Sun</strong> relies on nuclear fusion,<br />

turning hydrogen into helium.<br />

Nuclear Fusion<br />

The <strong>15</strong> million K plasma in the solar core is like a “soup”<br />

of hot gas, with bare, positively charged atomic nuclei (and<br />

negatively charged electrons) whizzing about at extremely<br />

high speeds. At any one time, some of these nuclei are on<br />

high-speed collision courses with each other. In most cases,<br />

electromagnetic forces deflect the nuclei, preventing actual<br />

collisions, because positive charges repel one another. If<br />

nuclei collide with sufficient energy, however, they can stick<br />

together to form a heavier nucleus (Figure <strong>15</strong>.6).<br />

Sticking positively charged nuclei together is not easy.<br />

The strong force,which binds protons and neutrons together<br />

in atomic nuclei, is the only force in nature that can<br />

At low speeds, electromagnetic<br />

repulsion prevents the collision<br />

of nuclei.<br />

At high speeds, nuclei come close<br />

enough for the strong force to bind<br />

them together.<br />

Figure <strong>15</strong>.6 Positively charged nuclei can fuse only if a highspeed<br />

collision brings them close enough for the strong force<br />

to come into play.<br />

chapter <strong>15</strong> • <strong>Our</strong> Star 501

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