Astronomy Principles and Practice Fourth Edition.pdf

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394 High energy instruments and other detectors Figure 23.12. The international Infrared Astronomical Satellite (IRAS) in preparation. (By permission of the Rutherford Appleton Laboratory.) Figure 23.13. The atmospheric windows for mm-astronomy. The dots indicate the frequencies corresponding to emissions from various molecular species. Full curve, Mauna Kea (predicted); broken curve, sea level. stationed on Mauna Kea mountain in Hawaii provides a 15 m dish made up of 276 separate panels of aluminium. Lightness of structure was achieved by pressing them from a honeycomb of lightweight aluminium and covering them with stretched aluminium sheets. Each panel is fixed to three motorized supports which can be controlled in positions to within ±3 µm so that the complete mirror is adjustable to the required parabolic shape. The collection aperture can be considered as an example of ‘active optics’. A special dome has been designed with a large slot to allow the collection dish an uninterrupted
Millimetre astronomy 395 Figure 23.14. The 15 m dish of the James Clerk Maxwell Telescope (JCMT) at Mauna Kea, Hawaii, without the protective membrane which normally fits between the large slit of the observing turret. (By permission of the Royal Observatory, Edinburgh.) view. However, the dish aperture is normally protected from the wind and from solar radiation by a large PTFE (polytetrafluoroethylene) membrane across the dome slit. This plastic sheet has a transmittance of 98% at mm wavelengths but absorbs 80% of the general solar radiation and allows observations to be made up to wind speeds of the order of 70 km h −1 . When the weather is calm, the shield can be removed to allow the most sensitive measurements which are degraded by the small amount of scattering that the membrane introduces. One of the chief instruments developed at the Royal Observatory, Edinburgh, and attached to the JMCT is SCUBA (Submillimetre Common-User Bolometer Array) which allows images to be obtained. The array of bolometers is cooled to 0·06 K making it the world’s most powerful submillimetre camera. It has had great success in mapping the centre of our galaxy, the galactic plane
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Chapter 1 Naked eye observations 1.
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A month 5 seen to rise above the ea
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A year 7 between south and west. An
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Chapter 2 Ancient world models Firs
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Ancient world models 11 Figure 2.1.
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Chapter 3 Observations made by inst
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Instrumentation in astronomy 15 Fig
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The role of the observer 17 Earth a
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Electromagnetic radiation 19 meteor
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Electromagnetic radiation 21 If, fo
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Electromagnetic radiation 23 device
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Direction of arrival of the radiati
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Brightness 27 Figure 5.3. The windo
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Brightness 29 physical conditions w
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Time 31 to house radio transmitters
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Chapter 6 The night sky 6.1 Star ma
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Simple observations 35 Figure 6.1.
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Chapter 7 The geometry of the spher
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Position on the Earth’s surface 4
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Position on the Earth’s surface 4
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Spherical trigonometry 51 determine
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Spherical trigonometry 53 Figure 7.
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The small spherical triangle 55 7.4
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Problems—Chapter 7 57 Although th
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Chapter 8 The celestial sphere: coo
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The equatorial system 61 Figure 8.2
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Circumpolar stars 63 Figure 8.4. A
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Also Hence, we have or The measurem
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The geocentric celestial sphere 67
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Transformation of one coordinate sy
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Right ascension 71 or cos 47 ◦ 39
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The Sun’s geocentric behaviour 73
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Sunset and sunrise 75 Figure 8.15.
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Megalithic man and the Sun 77 Figur
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The ecliptic system of coordinates
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Galactic coordinates 81 Table 8.1.
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Galactic coordinates 83 Figure 8.22
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Galactic coordinates 85 Figure 8.25
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Problems—Chapter 8 87 where ε is
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Sidereal time 89 Figure 9.1. The ti
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Sidereal time 91 Figure 9.3. An equ
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Mean solar time 93 Figure 9.4. Posi
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The relationship between mean solar
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The civil day and timekeeping 97 It
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The tropical year and the calendar
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The Earth’s geographical zones 10
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Hence, the period of the year durin
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Twilight 105 Figure 9.10. The heati
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Twilight 107 For this to happen, ZB
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h m s Date Approximate ZT 16 30 0 J
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Problems—Chapter 9 111 Date (00 h
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Atmospheric refraction 113 Figure 1
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where ZOL = r. But ZOL = ζ .AlsoAB
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so that we have But Hence, Similarl
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Now But θ is a small angle so we m
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Geocentric parallax 121 Figure 10.6
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The semi-diameter of a celestial ob
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Measuring distance in the Solar Sys
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Stellar parallax 127 Figure 10.10.
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Stellar parallax 129 after. The val
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Problems—Chapter 10 131 Recent ob
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Chapter 11 The reduction of positio
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The velocity of light 135 Table 11.
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The constant of aberration 137 Figu
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Diurnal and planetary aberration 13
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Precession of the equinoxes 141 Fig
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Effect of precession on a star’s
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Nutation 145 Figure 11.10. The grav
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The tropical and sidereal years 147
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Chapter 12 Geocentric planetary phe
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The Copernican System 151 Figure 12
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Planetary configurations 153 (a) V
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The synodic period 155 Figure 12.5.
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Measurement of planetary distances
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Stationary points 159 Figure 12.8.
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Stationary points 161 Using equatio
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The phase of a planet 163 Figure 12
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Problems—Chapter 12 165 with an o
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Planetary orbits 167 Figure 13.1. M
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Planetary orbits 169 If P 1 SP 2 is
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Newton’s law of gravitation 171 a
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The Principia of Isaac Newton 173 N
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The two-body problem 175 Figure 13.
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The two-body problem 179 13.6.5 The
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The astronomical unit 183 For an ex
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Chapter 14 Celestial mechanics: the
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14.3 General properties of the many
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Special perturbation theories 189 F
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Special perturbation theories 191 F
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14.6 Dynamics of artificial Earth s
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The geostationary satellite 195 in
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Interplanetary transfer orbits 197
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Then V B = V c2 − V A ,sinceV c2
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Problems—Chapter 14 205 (figure 1
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210 The radiation laws Figure 15.1.
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212 The radiation laws Table 15.1.
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216 The radiation laws In order to
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218 The radiation laws where σ is
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220 The radiation laws The brightne
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222 The radiation laws centrifugal
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226 The radiation laws is moving pa
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230 The radiation laws In most phys
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232 The radiation laws radiation ha
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234 The radiation laws radiation is
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236 The radiation laws Figure 15.14
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Chapter 16 The optics of telescope
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240 The optics of telescope collect
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Chapter 17 Visual use of telescopes
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274 Visual use of telescopes By sub
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276 Visual use of telescopes 17.3 M
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278 Visual use of telescopes By let
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280 Visual use of telescopes Figure
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282 Visual use of telescopes For sm
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284 Detectors for optical telescope
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306 Astronomical optical measuremen
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Chapter 20 Modern telescopes and ot
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332 Modern telescopes and other opt
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Page 340 and 341: 344 Modern telescopes and other opt
Page 348 and 349: Chapter 21 Radio telescopes 21.1 In
Page 350 and 351: 354 Radio telescopes Figure 21.2. A
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Page 358 and 359: 362 Radio telescopes (a) Paraboloid
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Page 362 and 363: 366 Radio telescopes The record fro
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Page 370 and 371: Chapter 22 Telescope mountings 22.1
Page 372 and 373: 376 Telescope mountings arc and thi
Page 374 and 375: 378 Telescope mountings Figure 22.4
Page 376 and 377: 380 Telescope mountings The design
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Page 398 and 399: 404 Practical projects to give the
Page 400 and 401: 406 Practical projects Figure 24.2.
Page 402 and 403: 408 Practical projects measurement
Page 410 and 411: 416 Practical projects Summer Time
Page 412 and 413: 418 Practical projects Figure 24.12
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Page 422 and 423: 428 Practical projects 24.5 Solar d
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Page 426 and 427: 432 Practical projects 24.5.4 The e
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Page 434 and 435: 440 Practical projects Table 24.2.
Page 436 and 437: 442 Practical projects 24.7.2 The i
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446 Practical projects Figure 24.30
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448 Practical projects right ascens
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450 Practical projects amenable to
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452 Web sites • W 20.5—www.mrao
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Appendix: Astronomical and related
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456 Appendix: Astronomical and rela
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Bibliography 1 Source books The Ast
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Answers to problems Chapter 7 1. 32
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462 Answers to problems Figure A8.2
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464 Answers to problems Figure A10.
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466 Answers to problems Figure A13.
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468 Answers to problems 5. 1·64 6.
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470 Index black body radiation, 216
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472 Index atom, 221 line, 353 illum
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474 Index potential energy, 177 pow
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