Gravitational Physics of Stellar and Galactic SystemsCambridge University Press, 1987/07/31 - 512 ページ This text describes the gravitational interactions and evolution of astronomical systems on all scales, from small groups of stars through galaxies and clusters of galaxies to the Universe itself. In a rapidly developing area of astronomy, it is the first comprehensive treatise on the subject to be published since the early 1960s. Concentrating on the basic physics, at a graduate student level, it also develops many astronomical applications in considerable detail. The book is self-contained. Most results are derived from preceding ones in a straightforward way. It is written to bring out the physical content behind the mathematical formulae, and contains a number of exercises and suggestions for research topics. Bibliographies with nearly 300 selected references provide gateways into the literature. |
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ix ページ
... models 290 40.1 . Polytropes and isothermal spheres 290 40.2 . Loaded polytropes 294 40.3 . Fokker - Planck models 299 41 Applying the virial theorem 303 42 Observed dynamical properties of clusters 312 42.1 . Clusters of galaxies 313 ...
... models 290 40.1 . Polytropes and isothermal spheres 290 40.2 . Loaded polytropes 294 40.3 . Fokker - Planck models 299 41 Applying the virial theorem 303 42 Observed dynamical properties of clusters 312 42.1 . Clusters of galaxies 313 ...
x ページ
... Models of thick disks 474 66.5 . Origin of the density profiles of elliptical galaxies 474 66.6 . Orbits and adiabatic invariants in a triaxial galaxy 475 67 Unanswered questions 476 68 Bibliography 478 Index 481 Preface The plan of ...
... Models of thick disks 474 66.5 . Origin of the density profiles of elliptical galaxies 474 66.6 . Orbits and adiabatic invariants in a triaxial galaxy 475 67 Unanswered questions 476 68 Bibliography 478 Index 481 Preface The plan of ...
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目次
III | 1 |
IV | 3 |
V | 7 |
VI | 14 |
VII | 21 |
VIII | 29 |
IX | 34 |
X | 39 |
LXV | 259 |
LXVI | 263 |
LXVII | 265 |
LXVIII | 270 |
LXIX | 272 |
LXX | 277 |
LXXI | 280 |
LXXII | 281 |
XI | 44 |
XII | 49 |
XIII | 54 |
XIV | 64 |
XV | 69 |
XVI | 73 |
XVII | 77 |
XVIII | 86 |
XIX | 90 |
XX | 95 |
XXI | 96 |
XXII | 100 |
XXIII | 105 |
XXIV | 107 |
XXV | 114 |
XXVI | 117 |
XXVII | 119 |
XXVIII | 124 |
XXIX | 127 |
XXX | 128 |
XXXI | 130 |
XXXIII | 131 |
XXXIV | 135 |
XXXV | 137 |
XXXVI | 143 |
XXXVII | 147 |
XXXVIII | 151 |
XXXIX | 158 |
XL | 163 |
XLI | 171 |
XLII | 175 |
XLIII | 178 |
XLIV | 181 |
XLV | 185 |
XLVI | 195 |
XLVII | 202 |
XLVIII | 206 |
XLIX | 209 |
L | 213 |
LI | 215 |
LII | 218 |
LIII | 220 |
LIV | 222 |
LV | 226 |
LVI | 228 |
LVII | 230 |
LVIII | 233 |
LIX | 238 |
LX | 245 |
LXII | 249 |
LXIII | 255 |
LXIV | 256 |
LXXIII | 287 |
LXXIV | 290 |
LXXV | 294 |
LXXVI | 299 |
LXXVII | 303 |
LXXVIII | 312 |
LXXIX | 313 |
LXXX | 316 |
LXXXI | 318 |
LXXXII | 321 |
LXXXIII | 328 |
LXXXIV | 335 |
LXXXV | 340 |
LXXXVI | 346 |
LXXXVII | 352 |
LXXXVIII | 356 |
LXXXIX | 362 |
XC | 365 |
XCI | 369 |
XCII | 374 |
XCIII | 378 |
XCIV | 382 |
XCV | 385 |
XCVI | 387 |
XCVII | 388 |
XCVIII | 389 |
391 | |
CI | 397 |
CII | 399 |
CIII | 406 |
CIV | 410 |
CV | 414 |
CVI | 420 |
CVII | 427 |
CVIII | 438 |
CIX | 446 |
CX | 447 |
CXI | 450 |
CXII | 453 |
CXIII | 456 |
CXIV | 461 |
CXV | 463 |
CXVI | 466 |
CXVII | 471 |
CXVIII | 473 |
CXIX | 474 |
CXX | 475 |
CXXI | 476 |
478 | |
481 | |
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多く使われている語句
Aarseth amplitude angular momentum approximation average basic BBGKY hierarchy becomes binary clusters of galaxies collisionless Boltzmann equation collisions components constant coordinates core correlation function decreases density distribution depends derivative described detailed disk distribution function dominate dynamical dynamical friction effects ensemble entropy equilibrium evolution evolve example expansion finite fluctuations Fokker-Planck Fokker-Planck equation force Fourier galaxy clustering gives globular clusters gravitating systems halo homogeneous inhomogeneity instability integral interactions kinetic energy linear Liouville's equation luminosity mass massive star microcells models motion N-body simulations non-linear objects observed orbits parameters particles perturbations phase space physical Poisson's equation polytropes potential energy probability problem radial radius random ratio region relation result rotation Saslaw scale scattering Section shows solution spatial spherical spiral stellar system structure symmetry temperature thermodynamics tidal timescale total energy velocity dispersion velocity distribution violent relaxation virial theorem volume waves zero