Summary

While most amateur astronomers know about the red shift, have a general idea of the way that the emission and absorption lines in stellar spectra provide an insight into the atomic processes of the star, it is unusual to find someone who has any kind of detailed knowledge. The reason isn't lack on interest - far from it - but is because all the books currently available are pitched at professional astronomers and degree students, and are to say the least, difficult to read.

This is the first non-technical book on this subject, written specifically for practical amateur astronomers. It includes all the science necessary for a qualitative understanding of stellar spectra, but avoids a mathematical treatment which would alienate many of its intended readers.

Any amateur astronomer who carries out (or who is interested in) observational spectroscopy and who wants a non-technical account of the physical processes which determine the intensity and profile morphology of lines in stellar spectra will find this is the only book written specially for him. And of course, "armchair astronomers" who simply want to understand the physical processes which shape lines in stellar spectra will find this book equally fascinating.

Choice Review

A significant scientific achievement of the 20th century was the elucidation of the nature of stars. This breakthrough required the interpretation of stellar spectra, i.e., the amount of energy that a star radiates as a function of the wavelength at which the star is observed. To understand spectra in detail requires advanced knowledge of physics. However, in this informative monograph, Robinson (Royal Astronomical Society) explains the basic concepts in terms that a general reader can master. Topics such as the characteristic radiation expected to be emitted by atoms, by ionized gas, and by molecules are addressed using illustrations and word descriptions of the physical processes. The section on curve of growth is challenging, and that on the Zeeman Effect involves a concept much beyond the rest of the book. It was disappointing that there was not a more extensive discussion of how these ideas could best be applied to actual data obtained by a skilled observer. For example, some Web sites providing lists of lines or sample spectra would have been helpful in illustrating the identification of lines in complicated spectra. Nonetheless, the interested reader will find this book a stimulating introduction. Summing Up: Recommended. General readers; lower-division undergraduates. D. E. Hogg emeritus, National Radio Astronomy Observatory