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 24
... direction defined by h . This also implies that the position and velocity vectors always lie in the same plane ( see Fig . 2.2 ) . Equation ( 2.6 ) is commonly referred to as the angular momentum integral . However , although h = | h ...
... direction defined by h . This also implies that the position and velocity vectors always lie in the same plane ( see Fig . 2.2 ) . Equation ( 2.6 ) is commonly referred to as the angular momentum integral . However , although h = | h ...
الصفحة 27
... direction Fig . 2.5 . The geometry of the ellipse of semi - major axis a , semi - minor axis b , eccentricity e , and longitude of pericentre w . Although a large number of cometary orbits have e≈ 1. 2.3 Orbital Position and Velocity 27.
... direction Fig . 2.5 . The geometry of the ellipse of semi - major axis a , semi - minor axis b , eccentricity e , and longitude of pericentre w . Although a large number of cometary orbits have e≈ 1. 2.3 Orbital Position and Velocity 27.
الصفحة 33
... directions are 2 ( ) 2 + ( ) 2 x = a ( cos E - e ) and y = a√1 - e2 sin E ( 2.41 ) ( cf. Eq . ( 2.21 ) ) . By adding the squares of these expressions and then taking the square root we have = Hence r = a ( 1 e cos E ) cos E - e 1- e ...
... directions are 2 ( ) 2 + ( ) 2 x = a ( cos E - e ) and y = a√1 - e2 sin E ( 2.41 ) ( cf. Eq . ( 2.21 ) ) . By adding the squares of these expressions and then taking the square root we have = Hence r = a ( 1 e cos E ) cos E - e 1- e ...
الصفحة 34
... direction ( see Fig . 2.5 ) . Colwell ( 1993 ) points out that papers have been published about the solution of Kepler's equation in virtually every decade since 1650 and that many eminent scientists have attempted solutions . Kepler's ...
... direction ( see Fig . 2.5 ) . Colwell ( 1993 ) points out that papers have been published about the solution of Kepler's equation in virtually every decade since 1650 and that many eminent scientists have attempted solutions . Kepler's ...
الصفحة 46
... direction to R2 , and hence ( ii ) the centre of mass is always on the line joining m1 and m2 , and we can write R1 + R2 = r , where r is the separation of my and m2 , and ( iii ) the distances of the masses from the centre of mass are ...
... direction to R2 , and hence ( ii ) the centre of mass is always on the line joining m1 and m2 , and we can write R1 + R2 = r , where r is the separation of my and m2 , and ( iii ) the distances of the masses from the centre of mass are ...
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