High Energy Astrophysics: Volume 2, Stars, the Galaxy and the Interstellar MediumCambridge University Press, 1992 - 412 pagine What role does viscosity play in accretion discs? How do you calculate the 'glitch function' of a pulsar? And can strong shocks account for the energy spectrum of electrons in our Galaxy? These are just some of the exciting questions that Professor Longair uses to develop the physics needed by the astronomer and high energy astrophysicist. The highly acclaimed first edition of High Energy Astrophysics instantly established itself as a classic in the teaching of contemporary astronomy. Reflecting the immense interest and developments in the subject, Professor Longair has developed the second edition into three texts; in this second volume he provides a comprehensive discussion of the high energy astrophysics of stars, the Galaxy and the interstellar medium. He develops an understanding for the essential physics with an elegance and infectious enthusiasm for which his teaching is internationally renowned, illustrating the issues throughout with results from forefront research. This book takes the student with a knowledge of physics and mathematics at the undergraduate level - but not necessarily with training in astronomy - to the point where current astronomical research can be understood. |
Sommario
III | 1 |
IV | 11 |
V | 14 |
VI | 17 |
VIII | 21 |
IX | 24 |
X | 34 |
XI | 40 |
LXII | 200 |
LXIII | 206 |
LXV | 209 |
LXVII | 210 |
LXVIII | 213 |
LXIX | 215 |
LXXII | 217 |
LXXIII | 221 |
XII | 41 |
XIII | 42 |
XIV | 46 |
XV | 52 |
XVI | 55 |
XVII | 57 |
XVIII | 63 |
XIX | 68 |
XX | 69 |
XXII | 75 |
XXIII | 84 |
XXIV | 87 |
XXV | 91 |
XXVI | 98 |
XXVII | 111 |
XXVIII | 115 |
XXIX | 119 |
XXX | 125 |
XXXI | 130 |
XXXII | 133 |
XXXIII | 136 |
XXXIV | 138 |
XXXV | 142 |
XXXVI | 143 |
XXXVII | 144 |
XXXVIII | 147 |
XXXIX | 150 |
XL | 151 |
XLI | 152 |
XLII | 153 |
XLIII | 154 |
XLV | 155 |
XLVI | 161 |
XLVIII | 167 |
XLIX | 168 |
L | 176 |
LI | 177 |
LII | 180 |
LIII | 181 |
LIV | 186 |
LV | 187 |
LVI | 191 |
LVII | 192 |
LVIII | 193 |
LIX | 194 |
LX | 198 |
LXI | 199 |
LXXIV | 229 |
LXXV | 230 |
LXXVI | 232 |
LXXVII | 236 |
LXXVIII | 239 |
LXXIX | 250 |
LXXX | 252 |
LXXXI | 256 |
LXXXII | 260 |
LXXXIII | 262 |
LXXXIV | 267 |
LXXXV | 270 |
LXXXVI | 274 |
LXXXVII | 278 |
LXXXVIII | 279 |
LXXXIX | 281 |
XC | 286 |
XCII | 288 |
XCIII | 292 |
XCIV | 296 |
XCV | 298 |
XCVI | 302 |
XCVII | 303 |
XCVIII | 306 |
XCIX | 307 |
C | 308 |
CI | 316 |
CII | 319 |
CIII | 322 |
CIV | 327 |
CV | 331 |
CVII | 333 |
CVIII | 343 |
CIX | 344 |
CX | 345 |
CXI | 346 |
CXII | 351 |
CXIII | 357 |
CXIV | 359 |
CXV | 362 |
CXVI | 363 |
CXVIII | 366 |
CXIX | 367 |
CXX | 370 |
CXXI | 374 |
382 | |
Parole e frasi comuni
absorption abundances acceleration accretion disc active galactic nuclei angle angular momentum Astrophys atoms binary systems black hole bremsstrahlung centre clusters collapse collisions compact star component cosmic rays diagram diffuse distance distribution dust elements emission lines emitted energy density energy loss energy spectrum equation evolution example explosion expression extragalactic Figure frequency Galaxy gravitational helium high energy astrophysics high energy electrons high energy particles hydrogen important infrared intensity interstellar gas interstellar medium ionised isotopes luminosity magnetic field magnetic field strength magnitude main sequence mass loss matter measured molecules Nebula neutrinos neutron star observed optical orbit physical plane plasma polarisation protons pulsars radio emission radio sources radius regions relativistic result Roche lobe rotation Section shown in Fig solar spallation spectra spiral stellar structure supernova remnants surface synchrotron radiation temperature timescale typical vector velocity volume waveband wavelengths waves white dwarfs X-ray binaries X-ray sources y-ray