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Introduction to Nanotechnology

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5.3. CARBON CLUSTERS 107<br />

-0 20 40 60 80 . 100 120<br />

Cluster Size N<br />

Figure 5.3. Mass spectrum of carbon clusters. The Cs0 and C70 fullerene peaks are evident.<br />

(With permission from S. Sugano and H. Koizuni, in Microcluster Physics, Springer-Verlag,<br />

Heidelberg, 1998.)<br />

the typical mass spectrum data obtained from such an experiment. For the number of<br />

a<strong>to</strong>ms N less than 30, there are clusters of every N, although some are more<br />

prominent than others. Calculations of the structure of small clusters by molecular<br />

orbital theory show the clusters have linear or closed nonplanar monocyclic<br />

geometries, as shown in Fig. 5.4. The linear structures that have sp hybridization<br />

occur when N is odd, and the closed structures form when N is even. The open<br />

structures with 3, 11, 15, 19, and 23 carbons have the usual bond angles and are<br />

more prominent and more stable. The closed structures have angles between the<br />

carbon bonds that differ from those predicted by the conventional hybridization<br />

concept. Notice in Fig. 5.3 that there is a very large mass peak at 60. The explanation<br />

of this peak and its structure earned a Nobel Prize.<br />

5.3.2. Discovery of Cs0<br />

The discovery of the existence of a soccer ball-like molecule containing 60 carbon<br />

a<strong>to</strong>ms was a somewhat fortui<strong>to</strong>us result of research on the nature of matter in outer<br />

space involving studies of light transmission through interstellar dust, the small<br />

particles of matter that fill the regions of outer space between stars and galaxies.<br />

When light from a distant star passes through the cosmos and arrives on Earth, the<br />

intensity of the light is reduced. This is referred <strong>to</strong> as optical extinction. It occurs<br />

because of the absorption and scattering of the light from the interstellar dust lying in

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