This book, written for a general readership, reviews and explains the three-body problem in historical context reaching to latest developments in computational physics and gravitation theory. The three-body problem is one of the oldest problems in science and it is most relevant even in today’s physics and astronomy.

The long history of the problem from Pythagoras to Hawking parallels the evolution of ideas about our physical universe, with a particular emphasis on understanding gravity and how it operates between astronomical bodies. The oldest astronomical three-body problem is the question how and when the moon and the sun line up with the earth to produce eclipses. Once the universal gravitation was discovered by Newton, it became immediately a problem to understand why these three-bodies form a stable system, in spite of the pull exerted from one to the other. In fact, it was a big question whether this system is stable at all in the long run.

Leading mathematiciansattacked this problem over more than two centuries without arriving at a definite answer. The introduction of computers in the last half-a-century has revolutionized the study; now many answers have been found while new questions about the three-body problem have sprung up. One of the most recent developments has been in the treatment of the problem in Einstein’s General Relativity, the new theory of gravitation which is an improvement on Newton’s theory. Now it is possible to solve the problem for three black holes and to test one of the most fundamental theorems of black hole physics, the no-hair theorem, due to Hawking and his co-workers.

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Mauri Valtonen has pioneered the study of the relativistic three-body problem and has worked on many of its applications in astronomical systems. He graduated at University of Cambridge in 1975, and has worked at University of Turku in Finland and in recent years at the University of the West Indies in Trinidad and Barbados. He has been awarded the E.J.Nystrom prize of the Finnish Society for Sciences and Letters.

Kiyotaka Tanikawa has initiated the numerical symbolic dynamics of the collinear and planar three-body problem. He graduated at the University of Tokyo in 1967 and has worked in the International Latitude Observatory until 1988, and then in the National Astronomical Observatory of Japan. He is retired Professor of the latter observatory and works there after retirement. Minor planet #10117 has been named after Tanikawa. He is also known as a historical astronomer using the ancient solar eclipses in order to determine the long-term variationsof the Earth rotation.

Victor Orlov is a graduate of Saint Petersburg State University. He joined studies of the three-body problem in 1975. Besides the three-body problem, his interests include the large-scale structure of the Universe, stellar dynamics, dynamics of multiple stars and galaxy groups. He is currently Professor of Saint Petersburg State University.

Aleksandr Myll�ri began the studies of the three-body problem in 1987 in Saint Petersburg State University. He has conducted joint research with all co-authors of the book. He is Associate Professor in St. George's University in Grenada, West Indies, and Adjunct Professor in �bo Akademi University in Finland.

Konstantin Kholshevnikov is a well known specialist in Celestial Mechanics. He has graduated in Saint Petersburg State University in 1962 and is currently the Head of Celestial Mechanics Chair of the same institute. His many awards include Leonhard Euler Medal of USSR Academy of Science, and the minor planet number 3504 is named after him.

Joanna Anosova is a pioneer in the study of the general three-body problem using computers. She is a graduate of Saint Petersburg State University, and has worked there for many decades. She is now retired Professor of University of Texas at Austin. The famous Agekian-Anosova map is named after her and her former teacher and colleague Tateos Agekian.

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