Solar System DynamicsCambridge University Press, 13 feb. 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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Pagina 8
... corresponding to widely spaced satellites . These results suggest that the apparent regular spacing of the orbital periods shown in Table 1.2 is not significant . There is no compelling evidence that the uranian satellite system is ...
... corresponding to widely spaced satellites . These results suggest that the apparent regular spacing of the orbital periods shown in Table 1.2 is not significant . There is no compelling evidence that the uranian satellite system is ...
Pagina 13
... corresponding to important resonances with Jupiter . The distribution of asteroids that have been discovered since Kirkwood's time show a number of cleared regions , most notably at the 4 : 1 , 3 : 1 , 5 : 2 , and 2 : 1 jovian ...
... corresponding to important resonances with Jupiter . The distribution of asteroids that have been discovered since Kirkwood's time show a number of cleared regions , most notably at the 4 : 1 , 3 : 1 , 5 : 2 , and 2 : 1 jovian ...
Pagina 20
... corresponding eccentricities e as 0.21001 , 0.00692 , 0.01800 , 0.09265 , 0.04822 , and 0.05700 , calculate the observed aphelion distance , a ( 1 + e ) , of Mercury , Venus , and Earth and the perihelion distance , a ( 1 − e ) , of ...
... corresponding eccentricities e as 0.21001 , 0.00692 , 0.01800 , 0.09265 , 0.04822 , and 0.05700 , calculate the observed aphelion distance , a ( 1 + e ) , of Mercury , Venus , and Earth and the perihelion distance , a ( 1 − e ) , of ...
Pagina 24
... corresponding to 0 = 0. Note that even though the centre of mass of m1 and m2 could be moving in inertial space , the direction of the reference line remains fixed . If we let ↑ and ô denote unit vectors along and perpendicular to the ...
... corresponding to 0 = 0. Note that even though the centre of mass of m1 and m2 could be moving in inertial space , the direction of the reference line remains fixed . If we let ↑ and ô denote unit vectors along and perpendicular to the ...
Pagina 59
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Cuprins
LXVIII | 261 |
LXIX | 264 |
LXX | 270 |
LXXI | 274 |
LXXII | 279 |
LXXIII | 283 |
LXXIV | 289 |
LXXV | 293 |
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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 |
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Termeni și expresii frecvente
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