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. |
من داخل الكتاب
النتائج 1-5 من 82
الصفحة 21
... considering the fifteen possible ratios T / T ; ( i < j ) of orbital periods and the ten first - order ... Consider the study of the preference for commensurability in the solar system carried out by Roy & Ovenden ( see ...
... considering the fifteen possible ratios T / T ; ( i < j ) of orbital periods and the ten first - order ... Consider the study of the preference for commensurability in the solar system carried out by Roy & Ovenden ( see ...
الصفحة 23
... consider the motion of m2 with respect to my . This allows us to simplify the problem without losing any of its essential features . In Sect . 2.7 we shall revert to considering motion in the centre of mass frame . Writing r = Ï1⁄2 ...
... consider the motion of m2 with respect to my . This allows us to simplify the problem without losing any of its essential features . In Sect . 2.7 we shall revert to considering motion in the centre of mass frame . Writing r = Ï1⁄2 ...
الصفحة 24
... consider this in more detail in Sect . 2.7 . Since r and r always lie in the same plane ( the orbit plane ) it is natural that we now restrict ourselves to considering motion in that plane ; the motion referred to an arbitrary reference ...
... consider this in more detail in Sect . 2.7 . Since r and r always lie in the same plane ( the orbit plane ) it is natural that we now restrict ourselves to considering motion in that plane ; the motion referred to an arbitrary reference ...
الصفحة 29
... Consider the case of two objects of mass m and m ' , orbiting a central object of mass me . Let the orbiting objects have semi - major axes a and a ' and orbital periods T and T ' . Equation ( 2.22 ) gives mc + m mc + m ' = m + m ' mc + ...
... Consider the case of two objects of mass m and m ' , orbiting a central object of mass me . Let the orbiting objects have semi - major axes a and a ' and orbital periods T and T ' . Equation ( 2.22 ) gives mc + m mc + m ' = m + m ' mc + ...
الصفحة 43
... Consider the true elliptical path of P and denote the angle FÊ'P by g . Applying the cosine rule to the triangle FF'P we obtain ( 1 − r / a ) + e2 e ( 1 - r / a ) + e ' ( 2.98 ) ( 2.100 ) ( 2.102 ) ( 2.103 ) 1 and hence F ' ≈e cos M g ...
... Consider the true elliptical path of P and denote the angle FÊ'P by g . Applying the cosine rule to the triangle FF'P we obtain ( 1 − r / a ) + e2 e ( 1 - r / a ) + e ' ( 2.98 ) ( 2.100 ) ( 2.102 ) ( 2.103 ) 1 and hence F ' ≈e cos M g ...
المحتوى
LXVIII | 261 |
LXIX | 264 |
LXX | 270 |
LXXI | 274 |
LXXII | 279 |
LXXIII | 283 |
LXXIV | 289 |
LXXV | 293 |
19 | |
22 | |
23 | |
25 | |
32 | |
37 | |
42 | |
45 | |
48 | |
XIX | 54 |
XX | 57 |
XXI | 60 |
XXII | 63 |
XXIII | 64 |
XXIV | 68 |
XXV | 71 |
XXVI | 74 |
XXVII | 77 |
XXVIII | 83 |
XXIX | 95 |
XXX | 97 |
XXXI | 102 |
XXXII | 107 |
XXXIII | 110 |
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 |
LXXXII | 318 |
LXXXIII | 321 |
LXXXIV | 326 |
LXXXV | 328 |
LXXXVI | 332 |
LXXXVII | 334 |
LXXXVIII | 337 |
LXXXIX | 341 |
XC | 364 |
XCI | 371 |
XCII | 373 |
XCIII | 375 |
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 |
CXII | 469 |
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