Yoshida, H. Recent Progress in the Theory and Application of Symplectic Integrators. Celestial Mechanics and Dynamical Astronomy 56 (1993) 27-43 Trobec, R., Merzel, F., Janezic, D. On the Complexity of Parallel Symplectic Molecular Dynamics Algorithms. J. Chem. Inf. Comput. Sci. 37 (1997) 1055-1062... [Pg.347]

Pierre Simon Laplace, the most influential of the French mathematician-scientists of his time, made many important contributions to celestial mechanics, the theory of heat, the mathematical theoiyi of probability, and other branches of pure and applied mathematics. lie was born into a Normandy family... [Pg.700]

The functions of the Academie Royal des Sciences were assumed in 1795 by a branch of the newly formed National Institute. Laplace was elected vice president of this reincarnated Academy and then elected president a few months later, in 1796. The duties of this position put him in contact with Napoleon Bonaparte. Three weeks after Napoleon seized power m 1799, Laplace presented him with copies of his work on celestial mechanics. Bonaparte quipped that he would read it in the first six weeks I have free and invited Laplace and his wife to dinner. Three weeks later, Napoleon named Laplace his minister of the interior. After six weeks, however, he was replaced Napoleon thought him a complete failure as an administrator. However, Napoleon continued to heap honors and rewards upon him, regarding him as a decoration of the state. lie made Laplace a chancellor of the Senate with a salai y that made him wealthy, named him to the Legion of Honor, and raised him to the rank of count of the empire. Laplace s wife was appointed a lady-in-waitmg to the Italian court of Napoleon s sister. Laplace responded with adulatory dedications of his works to Napoleon. [Pg.702]

The quote is from the third volume of Henri Poincare s New Methods of Celestial Mechanics, and is a description of his discovery of homoclinic orbits (see below) in the restricted three-body problem. It is also one of the earliest recorded formal observations that very complicated behavior may be found even in seemingly simple classical Hamiltonian systems. Although Hamiltonian (or conservative) chaos often involves fractal-like phase-space structures, the fractal character is of an altogether different kind from that arising in dissipative systems. An important common thread in the analysis of motion in either kind of dynamical system, however, is that of the stability of orbits. [Pg.188]

Only at the end of the 19th century did the first attempt to approach this subject systematically appear. In fact, Poincar6 became interested in certain problems in celestial mechanics,1 and this resulted in the famous small parameters method of which we shall speak in Part II of this chapter. In another earlier work2 Poincar6 investigated also certain properties of integral curves defined by ike differential equations of the nearly-linear class. [Pg.321]

Introductory Remarks.—As was mentioned in the introduction to this chapter, the quantitative part of the theory of Poincar6 was first applied in celestial mechanics.1 The two approaches the topological,2 and the analytical are unrelated in the original publications of Poincar6, and the connection between the two appeared nearly 50 years later when the theory of nonlinear oscillations was developed. [Pg.349]

In celestial mechanics difficulties were experienced in connection with the so-called secular terms, and at the end of the last century there was a tendency to get rid of these secular terms by a proper determination of the available constants (Lindstedt). [Pg.349]

In this work Poincar6 made a fundamental contribution by indicating a possibility of integrating certain nonlinear differential equations of celestial mechanics by power series in terms of certain parameters. We shall not give this theorem of Poincar614 but will briefly mention its applications. [Pg.349]

Perturbation theory is one of the oldest and most useful, general techniques in applied mathematics. Its initial applications to physics were in celestial mechanics, and its goal was to explain how the presence of bodies other than the sun perturbed the elliptical orbits of planets. Today, there is hardly a field of theoretical physics and chemistry in which perturbation theory is not used. Many beautiful, fundamental results have been obtained using this approach. Perturbation techniques are also used with great success in other fields of science, such as mathematics, engineering, and economics. [Pg.33]

In 1687, Newton summarized his discoveries in terrestrial and celestial mechanics in his Philosophiae naturalis principia mathematica (Mathematical Principles of Natural Philosophy), one of the greatest milestones in the history of science. In this work he showed how his (45) principle of universal gravitation provided an explanation both of falling bodies on the earth and of the motions of planets, comets, and other bodies in the heavens. The first part of the Principia, devoted to dynamics, includes Newton s three laws of motion the second part to fluid motion and other topics and the third part to the system of the (50) world, in which, among other things, he provides an explanation of Kepler s laws of planetary motion. [Pg.189]

See Kirrman s remarks, in Hommage a Albert Kirrman. And especially on Job, Albert Kirrmann, Notice sur les titres et travaux scientifiques(on 8), typescript of 20 pages, ENS, courtesy of ENS Bibliotheque des Lettres. Eugene Bloch taught physics at the Ecole Normale from 1913 on, and he became professor of theoretical physics and celestial mechanics at the Sorbonne in 1930. He succeeded Henri Abraham, one of Lespieau s old friends. [Pg.170]

Algebraic Geometry Antenna Theory Celestial Mechanics Computer-Aided Design Control Theory Deformation Analysis Econometrics... [Pg.103]

Jules) Henri Poincard, 1834-1912. French mathematician, physicist, and astronomer. Prolific and gifted writer on mathematical analysis, analytical and celestial mechanics, mathematical physics, and philosophy of science. [Pg.805]

The superiority of circular planetary orbits became almost a religious dogma in the Christian era, intimately tied to the idea of the perfection of God and of His creations. It was replaced by modem celestial mechanics only after centuries in which the concept of esthetic perfection of the universe was gradually superseded by a concept of esthetic perfection of a mathematical theory that could account for the... [Pg.3]

Euler s proof of the least action principle for a single particle (mass point in motion) was extended by Lagrange (c. 1760) to the general case of mutually interacting particles, appropriate to celestial mechanics. In Lagrange s derivation [436], action along a system path from initial coordinates P to final coordinates Q is defined by... [Pg.9]

A concept helpful for solving simple celestial mechanics problems is the centrifugal acceleration a of any body moving with a speed v in a circular orbit of radius r ... [Pg.27]

There is no analytical solution to the N-particle problem in quantum mechanics (neither is there one in, say, celestial mechanics or classical electrodynamics). The Hartree41-Fock42 approximation to the problem is to treat each electron individually, one at a time, in the average electrical field of all the other electrons and fixed nuclei. It yields the effective Hamiltonians (or Fock Hamiltonians) ... [Pg.159]

Lemaitre, A. Dubru, P 1991, Celestial Mechanics and Dynamical Astronomy, 52, 57. Levison, H. F. Agnor, C. 2003, Astronomical Journal, 125, 2692. [Pg.332]

Moons, M. Morbidelli, A. 1993, Celestial Mechanics and Dynamical Astronomy, 57,99. Morbidelli, A. 1999, Celestial Mechanics and Dynamical Astronomy, 73, 39. [Pg.333]

V. 1. Arnol d, V. V. Kozlov, and A. I. Neishtadt, Mathematical Aspects of Classical and Celestial Mechanics, Springer-Verlag, New York, 1988. [Pg.213]

H. Poincare, New Methods of Celestial Mechanics, Part 3, American Instimte of Physics, New York, 1993. [Pg.213]

As this book shows, TST is becoming more and more of a multidisciplinary endeavor. Some new applications may be found outside the realm of chemical physics. In particular, Marsden and co-workers [13] applied those concepts to celestial mechanics of small bodies, while the general theory of the Keplerian three-body problem makes use of TST, even if in a highly singular case [14,15]. Much work remains to be done outside of chemical physics types of dynamics. I come back to this question in the conclusion. [Pg.219]

The three-body problem appears in various physical and chemical systems—that is, celestial systems (e.g., the sun, the earth, and the moon), atomic systems (e.g., two electrons and one nucleus), and molecular systems (e.g., D + H2 DH + H reaction). Due to historical reasons, the three-body problem in celestial mechanics is the oldest. In order for our ancestors to make the calender, they observed the motion of the sun and the moon for agriculmral and fishery purposes and also for daily life. After Copernicus, they knew that the earth itself moves. But they did not know the law of the motion of stars and planets. By... [Pg.305]

In this section, mathematical results in celestial mechanics is reviewed. If the reader need a complete historical review, see Ref. 25. One of these results—that is, the McGehee s blow-up technique—will be used in Sections III and IV. [Pg.309]

In celestial mechanics, our attention focuses on the behavior of planets and/ or comets around the sun, which is described by the following Hamiltonian ... [Pg.309]

The McGehee s blow-up technique is essential to investigate the detailed structure of 7/-body problem in celestial mechanics. If the particles have a different sign of charge, such a Coulomb system has the same type of... [Pg.311]

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