Fundamental Astronomy

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

<strong>Fundamental</strong> <strong>Astronomy</strong>
Page 4 and 5: H. Karttunen P. Kröger H. Oja M. P
Page 6 and 7: Preface to the Fifth Edition As the
Page 8 and 9: Contents 1. Introduction 1.1 The Ro
Page 10 and 11: 9. Binary Stars and Stellar Masses
Page 12: Contents 20.9 Detecting life ......
Page 15 and 16: 4 1. Introduction on the locations
Page 17 and 18: 6 1. Introduction Fig. 1.4. The dim
Page 19 and 20: 8 1. Introduction Table 1.1. The sh
Page 21 and 22: 2. Spherical Astronomy Spherical as
Page 23 and 24: Fig. 2.5. The coordinates of the po
Page 25 and 26: zon equals the geographical latitud
Page 27 and 28: the object and the zenith, is obvio
Page 29 and 30: trigonometry. Comparing Figs. 2.6 a
Page 31 and 32: planes intersect along a straight l
Page 33 and 34: Table 2.1. For intervals longer tha
Page 35 and 36: where a is the altitude in degrees,
Page 37 and 38: Absolute coordinates are usually de
Page 39 and 40: If the source were at rest, the wav
Page 41 and 42: 2.12 Star Catalogues and Maps 31
Page 43 and 44: Earth. The rotation rate is slowly
Page 45 and 46: 2.14 Astronomical Time Systems Fig.
Page 47 and 48: Fig. 2.32. The difference between t
Page 49 and 50: Precession changes the ecliptic lon
Page 51 and 52: * Julian Date There are several met
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Example 2.5 Find the topocentric pl
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The Julian date is J = 2,445,074.5a
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48 3. Observations and Instruments
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84 4. Photometric Concepts and Magn
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5. Radiation Mechanisms In the prev
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Fig. 5.3. Polarization of light. Th
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series, which is in the ultraviolet
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Fig. 5.7. The Zeeman effect. In str
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electron whose energy is not quanti
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espect to λ and finding zero of th
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is not too high, we can use the Wie
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Substituting this into (5.39), we s
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It is quite difficult to listen to
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6. Celestial Mechanics Celestial me
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Fig. 6.3. The radial velocity ˙r i
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Fig. 6.5a-c. Six integration consta
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By comparing this with the length o
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The three-body problem has some int
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6.9 Escape Velocity If an object mo
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If the system remains bounded, i. e
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The energy integral (6.16) is now h
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coordinates of the Earth: X⊕ = 0.
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7. The Solar System The solar syste
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7.1 Planetary Configurations The ap
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sin a, where a is the altitude of t
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these points, the surface of the se
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Fig. 7.6. (a) A total solar eclipse
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the centrifugal force equal to the
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Fig. 7.12. The number of meteorite
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Fig. 7.13. (a) Temperature as a fun
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Fig. 7.16. Structure of the magneto
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Fig. 7.18. Planetary magnetic field
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7.8 Photometry, Polarimetry and Spe
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calculate only V(1,α)≡ V(1, 0)
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tem objects are also observed by me
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Fig. 7.23. (Left) A mosaic picture
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Fig. 7.25. Left: Venus in visible l
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surrounding an elevated plain, the
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Fig. 7.28. The tectonic plates. The
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Fig. 7.30. A map of the Lunar surfa
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Fig. 7.32. Structure of the Moon. T
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Fig. 7.33. Two pictures of Mars, ta
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7.14 Jupiter Fig. 7.36. The 360 deg
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Fig. 7.38. A composed image of Jupi
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Fig. 7.40. Mosaic of Jupiter’s ri
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Europa is the smallest of the Galil
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in Saturn’s atmosphere is only ab
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The Saturnian rings were possibly f
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Fig. 7.48. Left: The rings of Uranu
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Fig. 7.50. (Left) Neptune shows mor
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7.17 Minor Bodies of the Solar Syst
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Fig. 7.55. Left: Asteroid (951) Gas
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The images of asteroids (Fig. 7.55)
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estimations of the albedos, and the
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Fig. 7.63. Meteors are easy to capt
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This weak glow can be seen above th
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7.18 Origin of the Solar System Fig
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its to collide with planets or to b
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The size of the illuminated surface
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k1, k2 and k3 such that k1n1 + k2n2
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208 8. Stellar Spectra plate (or pe
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210 8. Stellar Spectra Fig. 8.3a,b.
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212 8. Stellar Spectra Fig. 8.5. Eq
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214 8. Stellar Spectra 8.4 Peculiar
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216 8. Stellar Spectra The HR diagr
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218 8. Stellar Spectra Fig. 8.9. Ma
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9. Binary Stars and Stellar Masses
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spectra show a regular variation. T
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Fig. 9.6. Typical lightcurves and s
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The secondary minimum is 4 5000
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230 10. Stellar Structure Fig. 10.2
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232 10. Stellar Structure - The tem
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234 10. Stellar Structure Fig. 10.4
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236 10. Stellar Structure compared
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238 10. Stellar Structure Table 10.
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240 10. Stellar Structure stars are
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242 10. Stellar Structure course th
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244 11. Stellar Evolution where G i
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246 11. Stellar Evolution Fig. 11.2
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250 11. Stellar Evolution the centr
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252 11. Stellar Evolution 11.5 The
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256 11. Stellar Evolution 11.7 Comp
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12. The Sun The Sun is our nearest
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The Solar Neutrino Problem. The cen
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12.2 The Atmosphere Fig. 12.4. Flas
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12.2 The Atmosphere Fig. 12.7. Prev
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Fig. 12.10. The Zürich sunspot num
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12.3 Solar Activity Fig. 12.13. Bec
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when the spots disappear. Apparentl
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12.5 Exercises Exercise 12.1 The so
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280 13. Variable Stars Fig. 13.2. T
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282 13. Variable Stars lations, if
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284 13. Variable Stars Table 13.2.
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286 13. Variable Stars Fig. 13.11.
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288 13. Variable Stars Fig. 13.13.
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290 13. Variable Stars The luminosi
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292 14. Compact Stars mainly due to
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294 14. Compact Stars to the surrou
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296 14. Compact Stars rotation peri
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298 14. Compact Stars now received
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300 14. Compact Stars Fig. 14.11. T
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302 14. Compact Stars time scale of
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304 14. Compact Stars In an X-ray b
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15. The Interstellar Medium Althoug
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and they will cover the fraction d
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If the particles in a cloud are ali
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ers first increase in the same way,
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Fig. 15.10. The reflection nebula N
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The Hubble relation can be derived
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Observable phenomenon Cause Interst
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Fig. 15.15. Interstellar absorption
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i. e. the brightness temperature im
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◭ Fig. 15.18. The great nebula in
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(atomic + molecular) between the ob
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T n [K] [cm −3 ] 1. Very cold mol
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is that passage through a spiral ar
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15.6 Supernova Remnants 333
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where B⊥ is the magnetic field co
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Fig. 15.27. The polarization of sta
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16. Star Clusters and Associations
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16.2 Open Star Clusters Fig. 16.2.
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Fig. 16.5. Colour-magnitude diagram
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Solving for the velocity we get v 2
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348 17. The Milky Way The basic dir
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350 17. The Milky Way of the releva
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352 17. The Milky Way Fig. 17.7. Th
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354 17. The Milky Way Table 17.1. P
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356 17. The Milky Way Fig. 17.13a-d
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358 17. The Milky Way longitude, as
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360 17. The Milky Way Fig. 17.19. R
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362 17. The Milky Way Later investi
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364 17. The Milky Way ments, some o
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366 17. The Milky Way The correspon
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368 18. Galaxies night sky. On the
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370 18. Galaxies Fig. 18.4. Differe
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372 18. Galaxies Fig. 18.6. M32 (ty
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374 18. Galaxies Masses. The distri
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376 18. Galaxies elliptical, normal
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378 18. Galaxies produced by supern
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380 18. Galaxies Fig. 18.12. Above:
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384 18. Galaxies Fig. 18.14. The la
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388 18. Galaxies Fig. 18.16. One of
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390 18. Galaxies Fig. 18.18. Galaxy
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19. Cosmology After the demise of t
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19.1 Cosmological Observations 395
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and Robert Wilson discovered that t
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19.3 Homogeneous and Isotropic Univ
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when the scale factor has increased
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On the other hand, using (19.26), q
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19.6 History of the Universe We hav
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using statistical methods. Perhaps
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Fig. 19.14. Angular power spectrum
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formed, or the star may be complete
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The third type of redshift is the g
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20. Astrobiology Is there life else
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RNA molecules have to carry instruc
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We have only recently started to un
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ing. Although this is too hot for l
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20.6 Are we Martians? Fig. 20.4. Th
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Fig. 20.5. A detailed image of the
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esearch, or OSETI, has already been
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Photograph on opposite page: Peculi
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A. Mathematics A.1 Geometry Units o
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434 A. Mathematics A.3 Taylor Serie
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436 A. Mathematics Scalar and vecto
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438 A. Mathematics matrix; thus the
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440 A. Mathematics This already sho
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442 B. Theory of Relativity can be
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444 B. Theory of Relativity Most of
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446 C. Tables Table C.3. Constants
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448 C. Tables Table C.9. Planets. R
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450 C. Tables Table C.13. Largest s
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452 C. Tables Table C.14. Some well
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454 C. Tables Table C.17. Nearest s
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456 C. Tables Table C.18. Brightest
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458 C. Tables Table C.21. Members o
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460 C. Tables Table C.23. Constella
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462 C. Tables Table C.25. Largest p
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464 C. Tables Table C.27. Some impo
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Answers to Exercises Chapter 2 2.1
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7.10 Assuming the comet rotates slo
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Further Reading The following list
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Shapiro, Teukolsky: Black Holes, Wh
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Photograph Credits We are grateful
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478 Name and Subject Index B Baade,
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480 Name and Subject Index dynamo 1
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482 Name and Subject Index horizon
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484 Name and Subject Index Mariner
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486 Name and Subject Index period-l
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488 Name and Subject Index slit spe
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490 Name and Subject Index - static
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492 Colour Supplement Photograph on
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494 Colour Supplement has made obse
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496 Colour Supplement Plate 3 Plate
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498 Colour Supplement Plate 8 Plate
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500 Colour Supplement Plate 12 Plat
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508 Colour Supplement Plate 30
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Fundamental Astronomy

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