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 10
... mean motion n in ° d - 1 is defined by n = 360 / T , where T is the orbital period of the body in days . The mean motions of Io , Europa , and Ganymede are nj = 203.488992435 ° d - 1 , ( 1.7 ) Fig . 1.5 . A montage of images of the ...
... mean motion n in ° d - 1 is defined by n = 360 / T , where T is the orbital period of the body in days . The mean motions of Io , Europa , and Ganymede are nj = 203.488992435 ° d - 1 , ( 1.7 ) Fig . 1.5 . A montage of images of the ...
الصفحة 11
... mean motions , nм and nte , is = 2.003139 . ( 1.12 ) ( 1.14 ) Enceladus and Dione are in a 2 : 1 orbit - orbit resonance and the ratio of their mean motions , ng and np , is given by ( 1.15 ) Fig . 1.6 . A Voyager 1 montage of Saturn ...
... mean motions , nм and nte , is = 2.003139 . ( 1.12 ) ( 1.14 ) Enceladus and Dione are in a 2 : 1 orbit - orbit resonance and the ratio of their mean motions , ng and np , is given by ( 1.15 ) Fig . 1.6 . A Voyager 1 montage of Saturn ...
الصفحة 15
... mean motions ( or average angular velocities ) of the two objects ( ni < n2 ) , using integers i1 , i2 € { 1 , 2 , ... , imax } with i1 < i2 and imax = 7 but excluding the case i = i2 = 1 , the 1 : 1 commensurability . However , the ...
... mean motions ( or average angular velocities ) of the two objects ( ni < n2 ) , using integers i1 , i2 € { 1 , 2 , ... , imax } with i1 < i2 and imax = 7 but excluding the case i = i2 = 1 , the 1 : 1 commensurability . However , the ...
الصفحة 16
... mean motions in the solar system . For example , the mean motions of the uranian satellites Miranda , Ariel , and Umbriel are 86.8688800 ° d - 1 , | π nм - 3nA + 2ny = -0.0785 ° d - 1 E F 0.15 ( 1.23 ) ( 1.24 ) ( 1.25 ) ( 1.26 ) Table ...
... mean motions in the solar system . For example , the mean motions of the uranian satellites Miranda , Ariel , and Umbriel are 86.8688800 ° d - 1 , | π nм - 3nA + 2ny = -0.0785 ° d - 1 E F 0.15 ( 1.23 ) ( 1.24 ) ( 1.25 ) ( 1.26 ) Table ...
الصفحة 17
... mean motions , that is , = 0.50035≈ 1 1/2 3/4 1/2 ニ( 1.27 ) Other examples of near - resonance among triads of mean motions in the solar system are shown in Table 1.3 . 2 Dermott ( 1973 ) has shown that there is a preference for ...
... mean motions , that is , = 0.50035≈ 1 1/2 3/4 1/2 ニ( 1.27 ) Other examples of near - resonance among triads of mean motions in the solar system are shown in Table 1.3 . 2 Dermott ( 1973 ) has shown that there is a preference for ...
المحتوى
LXVIII | 261 |
LXIX | 264 |
LXX | 270 |
LXXI | 274 |
LXXII | 279 |
LXXIII | 283 |
LXXIV | 289 |
LXXV | 293 |
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37 | |
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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 |
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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