Fundamental Astronomy

More documents

Recommendations

Info

$P 0.1 Stabilişti natura şsi suma seriilor: a) Σ 1 n\ ; b) Σ arctan 1 n# + n ...$

180 7. The Solar System The F ring, discovered in 1979, is about 3000 km outside A. The ring is only a few hundred kilometres wide. On both sides there is a small moon; these shepherds prevent the ring from spreading. An interior moon passing a ring particle causes the particle to move to a larger orbit. Similarly, at the outer edge of the ring, a second moon forces the particles inward. The net result is that the ring is kept narrow. Outside the F ring, there are some zones of very sparse material, sometimes referred to as the G and E rings. These are merely collections of small particles.
The Saturnian rings were possibly formed together with Saturn and are not debris from some cosmic catastrophe, like remnants of a broken moon. The total mass of the rings is 10 −7 of the mass of Saturn. If all ring particles were collected together, they would form an ice ball, 600 km in diameter. A total of 56 moons (late 2006) of Saturn are known. Many of the large Saturnian moons (Fig. 7.46) were observed by Pioneer 11 and Voyager 1 and 2 spacecrafts. Large moons (excluding Titan) are composed mainly of ice. The temperature of the primeval nebula at the distance of Saturn was so low that bodies of pure ice could form and survive. Some moons are dynamically interesting; some have an exotic geological past. Outside the F ring, there are two moonlets, Epimetheus and Janus, almost in the same orbit; the difference of the semimajor axes is about 50 km, less than the radii of the moons. The inner moon is gaining on the outer one. The moons will not collide, since the speed of the trailing moon increases and the moon moves outward. The speed of the leading moon decreases and it drops inward. The moons exchange their roles roughly every four years. There are also several shepherding satellites, like Atlas, Prometheus and Pandora that keep rings in their place. Their gravitational pull prevents ring particles from drifting away. The innermost of the “old” moons is Mimas. There is a huge crater on Mimas’ surface with a diameter of 100 km and a depth of 9 km (Fig. 7.46). Bigger craters exist in the solar system, but relative to the size of the parent body, this is almost the biggest crater there could be room for (otherwise the crater would be bigger than 7.16 Uranus and Neptune Fig. 7.46a–e. Saturnian moons photographed by the Cassini spacecraft in 2005–2006 (a) Hyperion, (b) Enceladus, (c) Iapetus and (d) Tethys.(e) A radar picture of the northern latitudes of Titan, taken by Cassini in summer 2006. The black patches are probably methane lakes. The width of the picture is about 450 km. (Photo NASA) Mimas itself). On the opposite side, some grooves can be seen, possibly signifying that impact has almost torn the moon apart. The surface of the next moon, Enceladus, consists of almost pure ice, and one side is nearly craterless. Craters and grooves can be found on the other hemisphere. Tidal forces result in volcanic activity where water (not lava or other “hot” material) is discharged to the surface. Titan is the largest of the Saturnian moons. Its diameter is 5150 km, so it is only slightly smaller than Jupiter’s moon Ganymede. Titan is the only moon with a dense atmosphere. The atmosphere is mainly nitrogen (98.4%) and methane, and the pressure at the surface is 1.5–2 bar. The temperature is about 90 K. Reddish clouds form the visible surface some 200 km above the solid body. Measurements and images of Huygens probe landing on Titan in 2005 did not reveal liquid methane lakes. However, Cassini orbiter radar data in 2006 strongly indicate the presence of the lakes (Fig. 7.44). An independent proof of liquids in the recent past can be seen in several surface features which possibly have been formed by flowing fluids. 7.16 Uranus and Neptune The planets from Mercury to Saturn were already known in antiquity. Uranus and Neptune can only be observed with a telescope. Uranus and Neptune are giants, similar to Jupiter and Saturn. Uranus. The famous German-English amateur astronomer William Herschel discovered Uranus in 1781. 181
Page 2:
Fundamental Astronomy
Page 5 and 6:
Dr. Hannu Karttunen University of T
Page 7 and 8:
VI Preface to the First Edition The
Page 9 and 10:
VIII Contents 5.6 Continuous Spectr
Page 11 and 12:
X Contents 16. Star Clusters and As
Page 14 and 15:
1. Introduction 1.1 TheRoleofAstron
Page 16 and 17:
1.2 Astronomical Objects of Researc
Page 18 and 19:
theory of relativity must be used t
Page 20 and 21:
of the gas may be 10 −21 kg m −
Page 22 and 23:
12 2. Spherical Astronomy angles co
Page 24 and 25:
14 or 2. Spherical Astronomy sin B
Page 26 and 27:
16 2. Spherical Astronomy defined t
Page 28 and 29:
18 2. Spherical Astronomy the verna
Page 30 and 31:
20 2. Spherical Astronomy pole. The
Page 32 and 33:
22 2. Spherical Astronomy Fig. 2.16
Page 34 and 35:
Page 36 and 37:
26 2. Spherical Astronomy
Page 38 and 39:
Page 40 and 41:
30 2. Spherical Astronomy numbers,
Page 42 and 43:
32 2. Spherical Astronomy In the 19
Page 44 and 45:
34 2. Spherical Astronomy mid-Septe
Page 46 and 47:
36 2. Spherical Astronomy correspon
Page 48 and 49:
38 2. Spherical Astronomy second of
Page 50 and 51:
2. Spherical Astronomy 40 Since ∆
Page 52 and 53:
42 2. Spherical Astronomy For the s
Page 54 and 55:
44 2. Spherical Astronomy red. What
Page 56 and 57:
3. Observations and Instruments Up
Page 58 and 59:
the long, oblique path through the
Page 60 and 61:
Fig. 3.6a-e. Diffraction and resolv
Page 62 and 63:
3.2 Optical Telescopes Fig. 3.10. T
Page 64 and 65:
3.2 Optical Telescopes Fig. 3.13. T
Page 66 and 67:
so thin that it absorbs very little
Page 68 and 69:
3.2 Optical Telescopes 59
Page 70 and 71:
3.2 Optical Telescopes 61
Page 72 and 73:
3.2 Optical Telescopes ◭ Fig. 3.1
Page 74 and 75:
and CCD-cameras have largely replac
Page 76 and 77:
Fig. 3.22a-e. The principle of read
Page 78 and 79:
than a prism. The dispersion can be
Page 80 and 81:
3.4 Radio Telescopes Fig. 3.25. The
Page 82 and 83:
Fig. 3.27. The Atacama Large Millim
Page 84 and 85:
Fig. 3.30. The VLA at Socorro, New
Page 86 and 87:
Fig. 3.31. (a) X-rays are not refle
Page 88 and 89:
Fig. 3.33. Refractors are not suita
Page 90 and 91:
tored by laser interferometers. If
Page 92 and 93:
4. Photometric Concepts and Magnitu
Page 94 and 95:
If we are outside the source, where
Page 96 and 97:
magnitudes can be equal, the flux d
Page 98 and 99:
flux L will now decrease with incre
Page 100 and 101:
this line is extrapolated to X = 0,
Page 102 and 103:
since due to extinction, radiation
Page 104 and 105:
96 5. Radiation Mechanisms Fig. 5.1
Page 106 and 107:
98 5. Radiation Mechanisms From (5.
Page 108 and 109:
100 5. Radiation Mechanisms Fig. 5.
Page 110 and 111:
Page 112 and 113:
104 5. Radiation Mechanisms We now
Page 114 and 115:
5. Radiation Mechanisms 106 Again F
Page 116 and 117:
Page 118 and 119:
110 5. Radiation Mechanisms We can
Page 120 and 121:
112 5. Radiation Mechanisms differe
Page 122 and 123:
114 6. Celestial Mechanics The solu
Page 124 and 125:
116 6. Celestial Mechanics prove (6
Page 126 and 127:
118 6. Celestial Mechanics in the d
Page 128 and 129:
120 6. Celestial Mechanics But cons
Page 130 and 131:
122 6. Celestial Mechanics by the e
Page 132 and 133:
124 6. Celestial Mechanics Substitu
Page 134 and 135:
126 6. Celestial Mechanics a cloud
Page 136 and 137:
128 6. Celestial Mechanics Since th
Page 138 and 139: 130 6. Celestial Mechanics Exercise
Page 140 and 141: 132 7. The Solar System Fig. 7.1. (
Page 142 and 143: 134 7. The Solar System for each ob
Page 144 and 145: 136 7. The Solar System Fig. 7.5. L
Page 146 and 147: 138 7. The Solar System Inserting t
Page 148 and 149: 140 7. The Solar System Therefore o
Page 150 and 151: 142 7. The Solar System Fig. 7.10.
Page 152 and 153: 144 7. The Solar System behaves mor
Page 154 and 155: 146 7. The Solar System Table 7.1.
Page 158 and 159: 150 7. The Solar System of the plan
Page 160 and 161: 152 7. The Solar System If we denot
Page 162 and 163: 154 7. The Solar System where F⊥
Page 166 and 167: 158 7. The Solar System larized fea
Page 170 and 171: 162 7. The Solar System The outer c
Page 176 and 177: 168 7. The Solar System weak and co
Page 178 and 179: 170 7. The Solar System amount of w
Page 184 and 185: 176 7. The Solar System ter the rin
Page 186 and 187: 178 7. The Solar System face, most
Page 190 and 191: 182 7. The Solar System Herschel hi
Page 196 and 197: 188 7. The Solar System liding, sin
Page 204 and 205: 196 7. The Solar System of this mat
Page 210 and 211: 202 7. The Solar System Near the po
Page 212 and 213: 204 7. The Solar System be solved f
Page 214 and 215: 8. Stellar Spectra All our informat
Page 216 and 217: which appears as irregular fluctuat
Page 218 and 219: 8.2 The Harvard Spectral Classifica
Page 220 and 221: ate of ionization is essentially de
Page 222 and 223: lines of titanium, scandium and van
Page 224 and 225: efore τ = 1, i. e. the radiation i
Page 226 and 227: yielding Iν(0,θ)= Sν(τ ∗ ) +
Page 228 and 229: 222 9. Binary Stars and Stellar Mas
Page 234 and 235: 10. Stellar Structure The stars are
Page 236 and 237: where a = 4σ/c = 7.564 × 10−16
Page 238 and 239:
where me is the electron mass and N
Page 240 and 241:
is produced by the proton-proton (p
Page 242 and 243:
oxygen, which in turn reacts to for
Page 244 and 245:
According to (4.7), (4.4) and (5.16
Page 246 and 247:
Example 10.6 The Radiation Pressure
Page 248 and 249:
11. Stellar Evolution In the preced
Page 250 and 251:
increases. The stellar surface temp
Page 252 and 253:
Since stars are most likely to be f
Page 254 and 255:
Fig. 11.4a-c. Energy transport in t
Page 256 and 257:
Fig. 11.5. The structure of a massi
Page 258 and 259:
tract to planetlike brown dwarfs. S
Page 260 and 261:
Fig. 11.10a-f. Evolution of a low-m
Page 262 and 263:
Fig. 11.12. The Wolf-Rayet star WR
Page 264 and 265:
In a neutron capture, a nucleus wit
Page 266 and 267:
This is several orders of magnitude
Page 268 and 269:
264 12.TheSun Fig. 12.2. (a) The ro
Page 270 and 271:
266 12.TheSun according to the heli
Page 272 and 273:
268 12.TheSun shines into view for
Page 274 and 275:
270 12.TheSun was established that
Page 276 and 277:
272 12.TheSun Fig. 12.11. In pairs
Page 278 and 279:
274 12.TheSun Fig. 12.15. (a) Quies
Page 280 and 281:
276 12.TheSun Fig. 12.17. An X-ray
Page 282 and 283:
13. Variable Stars Stars with chang
Page 284 and 285:
Fig. 13.3. The variation of brightn
Page 286 and 287:
Fig. 13.5. The lightcurve of a long
Page 288 and 289:
duced when the carbon condenses int
Page 290 and 291:
13.3 Eruptive Variables Fig. 13.12.
Page 292 and 293:
Fig. 13.15. Supernova 1987A in the
Page 294 and 295:
14. Compact Stars In astrophysics t
Page 296 and 297:
about 1.4 M⊙, which is thus the u
Page 298 and 299:
1968. In the following year it was
Page 300 and 301:
ditions required for hypernova expl
Page 302 and 303:
This is greater than the speed of l
Page 304 and 305:
Fig. 14.12. Scale drawings of 16 bl
Page 306 and 307:
are (or, in the radio case, have on
Page 308 and 309:
14.6 Exercises Exercise 14.1 The ma
Page 310 and 311:
308 15. The Interstellar Medium Fig
Page 312 and 313:
310 15. The Interstellar Medium R d
Page 314 and 315:
312 15. The Interstellar Medium pol
Page 316 and 317:
Page 318 and 319:
Page 320 and 321:
318 15. The Interstellar Medium Tab
Page 322 and 323:
Page 324 and 325:
322 15. The Interstellar Medium met
Page 326 and 327:
324 15. The Interstellar Medium
Page 328 and 329:
326 15. The Interstellar Medium He
Page 330 and 331:
Page 332 and 333:
330 15. The Interstellar Medium up
Page 334 and 335:
332 15. The Interstellar Medium hav
Page 336 and 337:
334 15. The Interstellar Medium len
Page 338 and 339:
336 15. The Interstellar Medium dro
Page 340 and 341:
338 15. The Interstellar Medium the
Page 342 and 343:
340 16. Star Clusters and Associati
Page 344 and 345:
Page 346 and 347:
Page 348 and 349:
17. The Milky Way On clear, moonles
Page 350 and 351:
Fig. 17.3. The directions to the ga
Page 352 and 353:
classes of stars are main sequence
Page 354 and 355:
Fig. 17.9. The size of the volume e
Page 356 and 357:
lar material similarly moves in the
Page 358 and 359:
Fig. 17.14. In order to derive Oort
Page 360 and 361:
Fig. 17.17. The radial velocity as
Page 362 and 363:
a suitable mass distribution, such
Page 364 and 365:
esting because it may be a small-sc
Page 366 and 367:
material constituting the galaxy. I
Page 368 and 369:
18. Galaxies The galaxies are the f
Page 370 and 371:
Fig. 18.3. The classification of no
Page 372 and 373:
18.1 The Classification of Galaxies
Page 374 and 375:
Fig. 18.7. Compound luminosity func
Page 376 and 377:
In order to measure the mass at eve
Page 378 and 379:
length r0 = 1-5 kpc. In Sc galaxies
Page 380 and 381:
18.4 Dynamics of Galaxies We have s
Page 382 and 383:
gas. Some normal spirals may have b
Page 384 and 385:
the Large and Small Magellanic Clou
Page 386 and 387:
stars are forming and evolving into
Page 388 and 389:
panion galaxy. The tail is interpre
Page 390 and 391:
een made at these wavelengths with
Page 392 and 393:
galaxies in our present neighbourho
Page 394 and 395:
394 19. Cosmology tographs form an
Page 396 and 397:
396 19. Cosmology Fig. 19.3. Hubble
Page 398 and 399:
398 19. Cosmology element after hyd
Page 400 and 401:
400 19. Cosmology 19.3 Homogeneous
Page 402 and 403:
402 19. Cosmology The potential ene
Page 404 and 405:
404 19. Cosmology In an expanding c
Page 406 and 407:
406 19. Cosmology about 40,000 degr
Page 408 and 409:
408 19. Cosmology rather slowly. In
Page 410 and 411:
410 19. Cosmology Fig. 19.15. Corre
Page 412 and 413:
412 19. Cosmology where Ω0 = ρ0/
Page 414 and 415:
414 19. Cosmology Example 19.2 Find
Page 416 and 417:
416 20. Astrobiology According to t
Page 418 and 419:
418 20. Astrobiology of spiral gala
Page 420 and 421:
420 20. Astrobiology Fig. 20.2. Bla
Page 422 and 423:
422 20. Astrobiology reached 10% of
Page 424 and 425:
424 20. Astrobiology Now panspermia
Page 426 and 427:
426 20. Astrobiology 20.9 Detecting
Page 428 and 429:
428 20. Astrobiology cles that we s
Page 430 and 431:
Appendices 431
Page 432 and 433:
Ellipse. Equation in rectangular co
Page 434 and 435:
A and B can be determined graphical
Page 436 and 437:
When using matrix formalism it is c
Page 438 and 439:
Similarly, a volume integral I = f
Page 440 and 441:
B. Theory of Relativity Albert Eins
Page 442 and 443:
time interval between the events is
Page 444 and 445:
C. Tables Table C.1. SI basic units
Page 446 and 447:
Table C.6. The Sun Property Symbol
Page 448 and 449:
Table C.11. Osculating elements of
Page 450 and 451:
Discoverer Year of a Psid e i r M
Page 452 and 453:
Table C.16. Periodic comets with se
Page 454 and 455:
Table C.17 (continued) C. Tables Na
Page 456 and 457:
C. Tables Table C.19. Some double s
Page 458 and 459:
Table C.22. Optically brightest gal
Page 460 and 461:
Table C.23 (continued) Abbreviation
Page 462 and 463:
C. Tables Table C.26. Millimetre an
Page 464 and 465:
Table C.27 (continued) Satellite La
Page 466 and 467:
468 Answers to Exercises 6.2 a = 1.
Page 468 and 469:
470 Answers to Exercises Chapter 17
Page 470 and 471:
472 Further Reading Morrison (ed.):
Page 472 and 473:
474 Further Reading Maps and Catalo
Page 474 and 475:
Name and Subject Index A aberration
Page 476 and 477:
coherent radiation 95 Cold Dark Mat
Page 478 and 479:
forbidden transition 101, 332 four-
Page 480 and 481:
Kellman, Edith 212 Kepler’s equat
Page 482 and 483:
nautical mile 15 nautical triangle
Page 484 and 485:
Reber, Grote 69 recombination 95, 9
Page 486 and 487:
synchronous rotation 135 synchrotro
Page 488 and 489:
Colour Supplement 491
Page 490 and 491:
Plate 14. The first view from the s
Page 492 and 493:
Plate 1 Plate 2 Colour Supplement 4
Page 494 and 495:
Plate 6 Plate 5 Colour Supplement 4
Page 496 and 497:
Plate 9 Colour Supplement Plate 10
Page 498 and 499:
Page 500 and 501:
Page 502 and 503:
Plate 23 Plate 24 Colour Supplement
Page 504 and 505:
Colour Supplement Plate 29 507
Page 506 and 507:
show all

Fundamental Astronomy

You also want an ePaper? Increase the reach of your titles

Delete template?

Save as template?