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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النتائج 1-5 من 88
الصفحة 7
... obtain x = 0.0247 . However , it is not enough to be impressed by the seemingly remarkable fits . We need to subject the data to a statistical test and to calculate whether or not the value of x is small enough to be statistically ...
... obtain x = 0.0247 . However , it is not enough to be impressed by the seemingly remarkable fits . We need to subject the data to a statistical test and to calculate whether or not the value of x is small enough to be statistically ...
الصفحة 25
... obtain a scalar equation for the relative motion by substituting the expression for r from Eq . ( 2.7 ) into Eq . ( 2.5 ) ; comparing the f components gives μ ï - rė2 ( 2.11 ) To solve this equation and find r as a function of 0 we need ...
... obtain a scalar equation for the relative motion by substituting the expression for r from Eq . ( 2.7 ) into Eq . ( 2.5 ) ; comparing the f components gives μ ï - rė2 ( 2.11 ) To solve this equation and find r as a function of 0 we need ...
الصفحة 26
... obtain 1 du du u2 do de and hence Eq . ( 2.11 ) can be written ŕ -Ꮎ = -h u = and d2u r μ h2 The four possible conics are : circle : ellipse : parabola : hyperbola : + u = μ d02 h2 This is a second - order , linear differential equation ...
... obtain 1 du du u2 do de and hence Eq . ( 2.11 ) can be written ŕ -Ꮎ = -h u = and d2u r μ h2 The four possible conics are : circle : ellipse : parabola : hyperbola : + u = μ d02 h2 This is a second - order , linear differential equation ...
الصفحة 35
... obtain - E1 Mesin M , = 1 E2 = M + e sin ( M + e sin M ) ≈ M + e sin M + 1⁄2 e2 sin 2M , E3 = M + e sin ( M + e sin M + ≈ M + 12e2 si + ( e - e3 ) sin M + e2 sin 2M + ge ' ) = Ei + 1 = ∞ e2 sin 2M ) E ; for the first three steps ...
... obtain - E1 Mesin M , = 1 E2 = M + e sin ( M + e sin M ) ≈ M + e sin M + 1⁄2 e2 sin 2M , E3 = M + e sin ( M + e sin M + ≈ M + 12e2 si + ( e - e3 ) sin M + e2 sin 2M + ge ' ) = Ei + 1 = ∞ e2 sin 2M ) E ; for the first three steps ...
الصفحة 38
... obtained . If we write Eq . ( 2.52 ) as E - M = e sin E then , since E - M is an odd periodic function , it can be ... obtain Sπ Sπ bs ( e ) = 1 G Js ( se ) = π 2 36 ST JO π M ] √ S ST cos SM dM + = π ( 2.75 ) This integral can be ...
... obtained . If we write Eq . ( 2.52 ) as E - M = e sin E then , since E - M is an odd periodic function , it can be ... obtain Sπ Sπ bs ( e ) = 1 G Js ( se ) = π 2 36 ST JO π M ] √ S ST cos SM dM + = π ( 2.75 ) This integral can be ...
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