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Classifying stars is something of an art form that comes with practice. Each spectral class is defined by the spectrum of a standard star against which the other stars are compared. The classifier eventually memorizes the standards and can classify the spectrum of a random star very quickly. Annie Cannon classified well over 300,000 stars in her lifetime, one at a time. Modern classifiers are now heading toward automated systems that use computers and complex software to simulate what a human eye and mind can do.

The "single-line" concept has a powerful application in the discovery of planets orbiting other stars. In a double star system, each star affects the other and each revolves around a common center of mass. Each star therefore moves back and forth along the line of sight. Even a heavy planet in orbit about a star will make the star shift back and forth by a small amount. The Sun moves at a speed of about three meters per second as a result of Jupiter's pull. The amount by which a heavy planet will shift a star's spectrum is within the range of modern measurement. From such subtle reflexive motions, we infer the masses of tiny bodies, presumably of planets. Quite a number have now been found with masses roughly comparable to that of our Jupiter. We do not yet know what relation they bear to our own planets.

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