Chapter 15--Our Sun - Geological Sciences
Chapter 15--Our Sun - Geological Sciences
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