Solar System DynamicsCambridge University Press, 13/02/2000 The Solar System is a complex and fascinating dynamical system. This is the first textbook to describe comprehensively the dynamical features of the Solar System and to provide students with all the mathematical tools and physical models they need to understand how it works. It is a benchmark publication in the field of planetary dynamics and destined to become a classic. Clearly written and well illustrated, Solar System Dynamics shows how a basic knowledge of the two- and three-body problems and perturbation theory can be combined to understand features as diverse as the tidal heating of Jupiter's moon Io, the origin of the Kirkwood gaps in the asteroid belt, and the radial structure of Saturn's rings. Problems at the end of each chapter and a free Internet Mathematica® software package are provided. Solar System Dynamics provides an authoritative textbook for courses on planetary dynamics and celestial mechanics. It also equips students with the mathematical tools to tackle broader courses on dynamics, dynamical systems, applications of chaos theory and non-linear dynamics. |
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الصفحة i
... theory can be combined to understand features as diverse as the tidal heating of Jupiter's moon Io , the unusual rotation of Saturn's moon Hyperion , the origin of the Kirkwood gaps in the asteroid belt , the radial structure of ...
... theory can be combined to understand features as diverse as the tidal heating of Jupiter's moon Io , the unusual rotation of Saturn's moon Hyperion , the origin of the Kirkwood gaps in the asteroid belt , the radial structure of ...
الصفحة ix
... Theory for the Solar System Generalised Free and Forced Elements 7.12 Higher Order Secular Theory Exercise Questions Resonant Perturbations Introduction 8 8.1 8.2 8.3 8.4 Variation of Orbital Elements 8.5 Resonance in the Circular ...
... Theory for the Solar System Generalised Free and Forced Elements 7.12 Higher Order Secular Theory Exercise Questions Resonant Perturbations Introduction 8 8.1 8.2 8.3 8.4 Variation of Orbital Elements 8.5 Resonance in the Circular ...
الصفحة 18
... theory requires extensive algebraic manipulation . For example , the Fourier series expansion to fourth order in the eccentricity and inclination of the standard perturbing potential experienced by one orbiting body due to another ...
... theory requires extensive algebraic manipulation . For example , the Fourier series expansion to fourth order in the eccentricity and inclination of the standard perturbing potential experienced by one orbiting body due to another ...
الصفحة 19
... theory , set out to solve the important , practical problem of the gravitational interactions of a system of three orbiting bodies ( the three - body problem ) . Partly because of the new techniques he developed , dynamical systems theory ...
... theory , set out to solve the important , practical problem of the gravitational interactions of a system of three orbiting bodies ( the three - body problem ) . Partly because of the new techniques he developed , dynamical systems theory ...
الصفحة 44
... the point F ' , then we see that Ptolemy's scheme was accurate to order e . The triumph of Kepler was to produce a theory that was accurate to order e2 ( Hoyle 1974 ) . ( a ) ( d ) ܫܘ F m1 R1 44 2 The Two - Body Problem.
... the point F ' , then we see that Ptolemy's scheme was accurate to order e . The triumph of Kepler was to produce a theory that was accurate to order e2 ( Hoyle 1974 ) . ( a ) ( d ) ܫܘ F m1 R1 44 2 The Two - Body Problem.
المحتوى
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XXX | 97 |
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XXXIV | 115 |
XXXV | 121 |
XXXVI | 128 |
XXXVII | 130 |
XXXVIII | 131 |
XXXIX | 136 |
XL | 140 |
XLI | 149 |
XLII | 153 |
XLIII | 155 |
XLIV | 158 |
XLV | 160 |
XLVI | 166 |
XLVII | 174 |
XLVIII | 175 |
XLIX | 178 |
L | 183 |
LI | 186 |
LII | 189 |
LIII | 194 |
LIV | 200 |
LV | 210 |
LVI | 215 |
LVII | 217 |
LVIII | 222 |
LIX | 225 |
LX | 226 |
LXI | 228 |
LXII | 233 |
LXIII | 238 |
LXIV | 246 |
LXV | 248 |
LXVI | 251 |
LXVII | 253 |
LXXVI | 299 |
LXXVII | 302 |
LXXVIII | 307 |
LXXIX | 309 |
LXXX | 314 |
LXXXI | 317 |
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LXXXIII | 321 |
LXXXIV | 326 |
LXXXV | 328 |
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LXXXVII | 334 |
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XC | 364 |
XCI | 371 |
XCII | 373 |
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XCIV | 385 |
XCV | 387 |
XCVI | 390 |
XCVII | 394 |
XCVIII | 396 |
XCIX | 399 |
C | 402 |
CI | 405 |
CII | 406 |
CIII | 409 |
CIV | 410 |
CV | 413 |
CVI | 421 |
CVII | 428 |
CVIII | 448 |
CIX | 452 |
CX | 456 |
CXI | 466 |
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CXIII | 471 |
CXIV | 474 |
CXVII | 475 |
CXVIII | 481 |
CXIX | 492 |
CXX | 495 |
CXXI | 512 |
CXXII | 515 |
CXXIII | 518 |
CXXIV | 520 |
CXXV | 522 |
CXXVI | 524 |
CXXVII | 526 |
CXXVIII | 527 |
CXXIX | 529 |
CXXX | 530 |
CXXXI | 535 |
CXXXII | 539 |
CXXXIII | 557 |
CXXXIV | 577 |
طبعات أخرى - عرض جميع المقتطفات
عبارات ومصطلحات مألوفة
amplitude angle angular approach approximate argument associated assume asteroid body calculate centre chaotic circle circular close consider constant corresponding curves defined denote derived determined direction distance disturbing function dynamics Earth eccentricity effect encounter energy equal equations equilibrium points evolution example expansion expression follows force frame function given gives gravitational Hamiltonian Hence inclination increase initial inner integration Jupiter libration longitude mass mean motion moving Note numerical objects observed obtain occur orbit origin outer particle path pericentre period perturbations planet planetary plot position possible potential problem quantities radial radius reference relation resonance respectively ring rotating satellite Saturn Sect secular semi-major axis shown in Fig solar system solution stable surface Table theory tidal tide trajectory values variation vector write