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 75
الصفحة 23
... frame . Writing r = Ï1⁄2 − Ï1 , and using Eq . ( 2.1 ) , we obtain d2r + μ = dt2 r3 R = mim2 r3 0 , r2 r = m2r2 F2 ( 2.1 ) m2 ( 2.2 ) ( 2.5 ) Fig . 2.1 . A vector diagram for the forces acting on two masses , m1 and m2 , with position ...
... frame . Writing r = Ï1⁄2 − Ï1 , and using Eq . ( 2.1 ) , we obtain d2r + μ = dt2 r3 R = mim2 r3 0 , r2 r = m2r2 F2 ( 2.1 ) m2 ( 2.2 ) ( 2.5 ) Fig . 2.1 . A vector diagram for the forces acting on two masses , m1 and m2 , with position ...
الصفحة 24
... frame is considered in Sect . 2.8 . We now transform to a polar coordinate system ( r , 0 ) referred to an origin centred on the mass m1 and an arbitrary reference line corresponding to 0 = 0. Note that even though the centre of mass of ...
... frame is considered in Sect . 2.8 . We now transform to a polar coordinate system ( r , 0 ) referred to an origin centred on the mass m1 and an arbitrary reference line corresponding to 0 = 0. Note that even though the centre of mass of ...
الصفحة 37
... frame ( see Sect . 2.8 ) . This introduces considerable computational savings in numerical work . 2.5 Elliptic Expansions Since there are so few integrable problems in solar system dynamics , frequently we have to resort to ...
... frame ( see Sect . 2.8 ) . This introduces considerable computational savings in numerical work . 2.5 Elliptic Expansions Since there are so few integrable problems in solar system dynamics , frequently we have to resort to ...
الصفحة 42
... frame . This approach is also appropriate when considering systems such as perturbed motion in the vicinity of equilibrium points ( Sect . 3.8 ) , the effects of planetary oblateness on nearcircular , near - equatorial orbits ( Sect ...
... frame . This approach is also appropriate when considering systems such as perturbed motion in the vicinity of equilibrium points ( Sect . 3.8 ) , the effects of planetary oblateness on nearcircular , near - equatorial orbits ( Sect ...
الصفحة 49
... frame varies with time because of perturbations by other bodies ( see , for example , Standish et al . ( 1992 ) for a thorough discussion of coordinate systems and reference frames or Montenbruck ( 1989 ) for a set of coordinate ...
... frame varies with time because of perturbations by other bodies ( see , for example , Standish et al . ( 1992 ) for a thorough discussion of coordinate systems and reference frames or Montenbruck ( 1989 ) for a set of coordinate ...
المحتوى
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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 |
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LXXXIII | 321 |
LXXXIV | 326 |
LXXXV | 328 |
LXXXVI | 332 |
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LXXXVIII | 337 |
LXXXIX | 341 |
XC | 364 |
XCI | 371 |
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XCIII | 375 |
XCIV | 385 |
XCV | 387 |
XCVI | 390 |
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XCVIII | 396 |
XCIX | 399 |
C | 402 |
CI | 405 |
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CIII | 409 |
CIV | 410 |
CV | 413 |
CVI | 421 |
CVII | 428 |
CVIII | 448 |
CIX | 452 |
CX | 456 |
CXI | 466 |
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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