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Newton–Cartan theory (or geometrized Newtonian gravitation) is a geometrical re-formulation, as well as a generalization, of Newtonian gravity first introduced by Élie Cartan [1] [2] and Kurt Friedrichs [3] and later developed by G. Dautcourt, [4] W. G. Dixon, [5] P. Havas, [6] H. Künzle, [7] Andrzej Trautman, [8] and others.
The book is still considered influential in the physics community, with generally positive reviews, but with some criticism of the book's length and presentation style. To quote Ed Ehrlich: [4] 'Gravitation' is such a prominent book on relativity that the initials of its authors MTW can be used by other books on relativity without explanation.
Consequently, Einstein–Cartan theory is able to avoid the general-relativistic problem of the singularity at the Big Bang. [ 18 ] [ 19 ] The minimal coupling between torsion and Dirac spinors generates an effective nonlinear spin–spin self-interaction, which becomes significant inside fermionic matter at extremely high densities.
Theoretical physicist Rainer Sachs from the University of California, Berkeley, observed that The Large-Scale Structure of Space–Time was published within just a few years as Gravitation and Cosmology by Steven Weinberg and Gravitation by Charles Misner, Kip Thorne, and John Archibald Wheeler. He believed these three books can supplement each ...
The two-body problem in general relativity (or relativistic two-body problem) is the determination of the motion and gravitational field of two bodies as described by the field equations of general relativity. Solving the Kepler problem is essential to calculate the bending of light by gravity and the motion of a planet orbiting its sun.
Topics that deserve more attention include gravitational radiation and cosmology. However, this book can be supplemented by those by Misner, Thorne, and Wheeler, and by Weinberg. Smolin was teaching a course on general relativity to undergraduates as well as graduate students at Yale University using this book and felt satisfied with the ...
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The n-body problem is an ancient, classical problem [19] of predicting the individual motions of a group of celestial objects interacting with each other gravitationally. Solving this problem – from the time of the Greeks and on – has been motivated by the desire to understand the motions of the Sun, planets and the visible stars.