Once you have looked at the night sky on a moonless night it is not
hard to realise why so much of our science and religion has its
roots in the stars. Yet it took until 1850 to realise that fainter
stars were not necessarily further away, nor the brighter ones
closer. In fact within the magnitude range observable to the naked
eye it is probable that the brighter star is in fact further away.
Even today the measurement of stellar distances is relatively
difficult and is gener ally only done using dedicated telescopes.
In the early years of the 20th century Hertzsprung and Russell
developed a powerful classification diagram which al lows stars to
be distinguished using a plot of their colour versus magnitude. The
construction of this diagram involved the use of spectroscopy which
has become the cornerstone of modern astronomy. As telescopes
become more powerful, de tectors more sensitive and more physics is
added to astrophysics, astronomical spectroscopy becomes a more
powerful tool. The concern of this book is the spectral
classification of stars. With a single spectrum of a star it is
possible to uniquely classify an object and find its place on the
Hertzsprung-Russell diagram. This spectrum is thus equivalent to
having the colour and the magnitude of the object which can in turn
be related to mass and other quantities."
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