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 84
الصفحة 20
... given in Question 1.1 and the 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 ...
... given in Question 1.1 and the 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 ...
الصفحة 36
... given above , it is more efficient since ( a ) it can be programmed to make use of quantities that have already been calculated at each iteration and ( b ) it will converge faster . An important consideration in either of these ...
... given above , it is more efficient since ( a ) it can be programmed to make use of quantities that have already been calculated at each iteration and ( b ) it will converge faster . An important consideration in either of these ...
الصفحة 39
... given in Brouwer & Clemence ( 1961 ) . The series for r / a is given by O ( e3 ) . 3 ( sin 3M sin 3M - sin M ) = 1 - ecos M + ( 1 − cos 2M ) + - 2 Js ( se ) cos s M e4 ( cos 2M - cos 4M ) + O ( e3 ) . 3 3e3 8 ( cos M - cos 3M ) ( 2.79 ) ...
... given in Brouwer & Clemence ( 1961 ) . The series for r / a is given by O ( e3 ) . 3 ( sin 3M sin 3M - sin M ) = 1 - ecos M + ( 1 − cos 2M ) + - 2 Js ( se ) cos s M e4 ( cos 2M - cos 4M ) + O ( e3 ) . 3 3e3 8 ( cos M - cos 3M ) ( 2.79 ) ...
الصفحة 40
... given by COS E 10 + 22 S = 1 and = cos M + тез + e4 ( 9 ) ( 35 5 192 + e3 2 + e4 cos f = -e + + COS 4M ( cos 2M ( cos 2M -1 ) + sin ƒ = 2√√1 − e2 + et + e3 1 d $ 2 de COS M We can also use the series for r / a to derive the series ...
... given by COS E 10 + 22 S = 1 and = cos M + тез + e4 ( 9 ) ( 35 5 192 + e3 2 + e4 cos f = -e + + COS 4M ( cos 2M ( cos 2M -1 ) + sin ƒ = 2√√1 − e2 + et + e3 1 d $ 2 de COS M We can also use the series for r / a to derive the series ...
الصفحة 51
... given time , say September 25 , 1993 at 5.32 PM British Summer Time . Appendix A gives formulae for the calculation of the orbital elements of the planets at any time referred to the mean ecliptic and equinox of the epoch of noon on 1st ...
... given time , say September 25 , 1993 at 5.32 PM British Summer Time . Appendix A gives formulae for the calculation of the orbital elements of the planets at any time referred to the mean ecliptic and equinox of the epoch of noon on 1st ...
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