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 3
... vector from the Sun to a planet sweeps out equal areas in equal times . 3 ) The square of the orbital period of a planet is proportional to the cube of its semi - major axis . The geometry implied by the first two laws is illustrated in ...
... vector from the Sun to a planet sweeps out equal areas in equal times . 3 ) The square of the orbital period of a planet is proportional to the cube of its semi - major axis . The geometry implied by the first two laws is illustrated in ...
الصفحة 4
... vector . a2 and periods T1 and T2 , then T1 / T2 = ( a1 / a2 ) 3/2 , which is consistent with his original formulation of the law . m1m2 d2 It is important to remember that Kepler's laws were purely empirical : He had no physical ...
... vector . a2 and periods T1 and T2 , then T1 / T2 = ( a1 / a2 ) 3/2 , which is consistent with his original formulation of the law . m1m2 d2 It is important to remember that Kepler's laws were purely empirical : He had no physical ...
الصفحة 16
... vector Ĉi ( cos c , sin c ; ) and comparing the magnitude of the sum of the unit vectors , ĉ , with √N , where N is the number of vectors or ratios , we find that / √N = 1.01 , which 1.01 , which is not large enough to be interesting ...
... vector Ĉi ( cos c , sin c ; ) and comparing the magnitude of the sum of the unit vectors , ĉ , with √N , where N is the number of vectors or ratios , we find that / √N = 1.01 , which 1.01 , which is not large enough to be interesting ...
الصفحة 23
... vectors . If R = ( mir1 + m2r2 ) / ( m1 + m2 ) denotes the position vector of the centre of mass , then Eqs . ( 2.3 ) can be written at + b m1 + m2 ( 2.4 ) This implies that either the centre of mass is stationary ( if a = 0 ) or it is ...
... vectors . If R = ( mir1 + m2r2 ) / ( m1 + m2 ) denotes the position vector of the centre of mass , then Eqs . ( 2.3 ) can be written at + b m1 + m2 ( 2.4 ) This implies that either the centre of mass is stationary ( if a = 0 ) or it is ...
الصفحة 24
... vectors along and perpendicular to the radius vector respectively , then the position , velocity , and acceleration vectors can be written in polar coordinates as r = rî , r = rî + rôô , h ï = ( ï − rò2 ) î + J m1 rô2 ) ř + [ 1d ...
... vectors along and perpendicular to the radius vector respectively , then the position , velocity , and acceleration vectors can be written in polar coordinates as r = rî , r = rî + rôô , h ï = ( ï − rò2 ) î + J m1 rô2 ) ř + [ 1d ...
المحتوى
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 |
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