This book was first published in 2007. Variable stars are those that change brightness. Their variability may be due to geometric processes such as rotation, or eclipse by a companion star, or physical processes such as vibration, flares, or cataclysmic explosions. In each case, variable stars provide unique information about the properties of stars, and the processes that go on within them. This book provides a concise overview of variable stars, including a historical perspective, an introduction to stars in general, the techniques for discovering and studying variable stars, and a description of the main types of variable stars. It ends with short reflections about the connection between the study of variable stars, and research, education, amateur astronomy, and public interest in astronomy. This book is intended for anyone with some background knowledge of astronomy, but is especially suitable for undergraduate students and experienced amateur astronomers who can contribute to our understanding of these important stars.

Henry Norris Russell lived in two universes: that of his Presbyterian forebears and that of his science. Sharp-witted and animated by nervous energy, he became one of the most powerful voices in twentieth-century American astronomy, wielding that influence in calculated ways to redefine an entire science. He, more than any American of his generation, worked to turn an observation-centered discipline into a theory-driven pursuit centered on physics. Today, professional and amateur astronomers alike know Russell for the Hertzsprung-Russell diagram, the playing field for much of stellar astrophysics, as well as for his work on the evolution of stars and the origin of the solar system. But of far greater importance than his own research, which was truly remarkable in its own right, is Russell's stamp on the field as a whole. Functioning as a "headquarters scientist"--some called him General--Russell was an astronomer without a telescope. Yet he marshaled the data of the Hales and the Pickerings of the world, injected theory into mainstream astronomy, and brought atomic physics to its very core, often sparking controversy along the way. His students at Princeton went on to populate the most prestigious astronomical institutions in the United States, bringing with them Russell's beliefs that astronomy is really astrophysics and that researchers should be theoretically as well as empirically minded. This first-ever book-length biography of the "Dean of American Astronomers" interweaves personal and scientific history to illuminate how Russell's privileged Presbyterian family background, his education at Princeton and Cambridge, and his personal inclinations and attachments both served and were at odds with his campaign to modernize astronomy. This book will be of interest not only to astronomers and historians (particularly those interested in the emergence of astrophysics), but to anyone interested in the process of disciplinary change.

Focussing on the formulation of mathematical models for the light curves of eclipsing binary stars, and on the algorithms for generating such models, this book provides astronomers, both amateur and professional, with a guide for - specifying an astrophysical model for a set of observations - selecting an algorithm to determine the parameters of the model - estimating the errors of the parameters. It is written for readers with knowledge of basic calculus and linear algebra; appendices cover mathematical details on such matters as optimisation, co-ordinate systems, and specific models. While emphasising the physical and mathematical framework, the discussion remains close to the problems of actual implementation. The book concludes with chapters on specific models and approaches and the authors'views on the structure of future light-curve programs.

Eclipsing Variables - What They can Tell Us and What We can do with Them The aim of the present book will be to provide an introduction to the inter pretation of the observed light changes of eclipsing binary stars and their analysis for the elements of the respective systems. Whenever we study the properties of any celestial body - be it a planet or a star - all information we wish to gain can reach us through two different channels: their gravitational attraction, and their light. Gravitational interaction between our Earth and its celestial neighbours is, however, measurable only at distances of the order of the dimensions of our solar system; and the only means of communication with the realm of the stars are their nimble-footed photons reaching us - with appropriate time-lag - across the intervening gaps of space. As long as a star is single and emits constant light, it does not constitute a very revealing source of information. A spectrometry of its light can disclose, to be sure, the temperature (colour, or ionization) of the star's semi-transparent outer layers, their chemical composition, and prevalent pressure (through Stark effect) or magnetic field (Zeeman effect), it can disclose even some information about its absolute luminosity or rate of spin. It cannot, however, tell us anything about what we should like to know most - namely, the mass or size (i.e., density) of the respective configuration; its absolute dimensions, or its internal structure.