Fundamental Astronomy

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H. Karttunen P. Kröger H. Oja M. Poutanen K. J. Donner (Eds.) <strong>Fundamental</strong> <strong>Astronomy</strong> Fifth Edition With 449 Illustrations Including 34 Colour Plates and 75 Exercises with Solutions 123
Dr. Hannu Karttunen University of Turku, Tuorla Observatory, 21500 Piikkiö, Finland e-mail: hannu.karttunen@utu.fi Dr. Pekka Kröger Isonniitynkatu 9 C 9, 00520 Helsinki, Finland e-mail: pekka.kroger@stadia.fi Dr. Heikki Oja Observatory, University of Helsinki, Tähtitorninmäki (PO Box 14), 00014 Helsinki, Finland e-mail: heikki.oja@helsinki.fi Dr. Markku Poutanen Finnish Geodetic Institute, Dept. Geodesy and Geodynamics, Geodeetinrinne 2, 02430 Masala, Finland e-mail: markku.poutanen@fgi.fi Dr. Karl Johan Donner Observatory, University of Helsinki, Tähtitorninmäki (PO Box 14), 00014 Helsinki, Finland e-mail: donner@astro.helsinki.fi ISBN 978-3-540-34143-7 5th Edition Springer Berlin Heidelberg New York ISBN 978-3-540-00179-9 4th Edition Springer-Verlag Berlin Heidelberg New York Library of Congress Control Number: 2007924821 Cover picture: The James Clerk Maxwell Telescope. Photo credit: Robin Phillips and Royal Observatory, Edinburgh. Image courtesy of the James Clerk Maxwell Telescope, Mauna Kea Observatory, Hawaii Frontispiece: The Horsehead Nebula, officially called Barnard 33, in the constellation of Orion, is a dense dust cloud on the edge of a bright HII region. The photograph was taken with the 8.2 meter Kueyen telescope (VLT 2) at Paranal. (Photograph European Southern Observatory) Title of original Finnish edition: Tähtitieteen perusteet (Ursan julkaisuja 56) © Tähtitieteellinen yhdistys Ursa Helsinki 1984, 1995, 2003 Sources for the illustrations are given in the captions and more fully at the end of the book. Most of the uncredited illustrations are © Ursa Astronomical Association, Raatimiehenkatu 3A2, 00140 Helsinki, Finland This work is subject to copyright. All rights are reserved, whether the whole or part of the material is concerned, specifically the rights of translation, reprinting, reuse of illustrations, recitation, broadcasting, reproduction on microfilm or in any other way, and storage in data banks. Duplication of this publication or parts thereof is permitted only under the provisions of the German Copyright Law of September 9, 1965, in its current version, and permission for use must always be obtained from Springer-Verlag. Violations are liable for prosecution under the German Copyright Law. Springer is a part Springer Science+Business Media www.springer.com © Springer-Verlag Berlin Heidelberg 1987, 1994, 1996, 2003, 2007 The use of general descriptive names, registered names, trademarks, etc. in this publication does not imply, even in the absence of a specific statement, that such names are exempt from the relevant protective laws and regulations and therefore free for general use. Typesetting and Production: LE-TeX, Jelonek, Schmidt & Vöckler GbR, Leipzig Cover design: Erich Kirchner, Heidelberg/WMXDesign, Heidelberg Layout: Schreiber VIS, Seeheim Printed on acid-free paper SPIN: 11685739 55/3180/YL 5 43210
Page 2: Fundamental Astronomy
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 36 and 37: 26 2. Spherical Astronomy
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
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44 2. Spherical Astronomy red. What
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3. Observations and Instruments Up
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the long, oblique path through the
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Fig. 3.6a-e. Diffraction and resolv
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3.2 Optical Telescopes Fig. 3.10. T
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3.2 Optical Telescopes Fig. 3.13. T
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so thin that it absorbs very little
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3.2 Optical Telescopes 59
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3.2 Optical Telescopes 61
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3.2 Optical Telescopes ◭ Fig. 3.1
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and CCD-cameras have largely replac
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Fig. 3.22a-e. The principle of read
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than a prism. The dispersion can be
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3.4 Radio Telescopes Fig. 3.25. The
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Fig. 3.27. The Atacama Large Millim
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Fig. 3.30. The VLA at Socorro, New
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Fig. 3.31. (a) X-rays are not refle
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Fig. 3.33. Refractors are not suita
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tored by laser interferometers. If
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4. Photometric Concepts and Magnitu
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If we are outside the source, where
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magnitudes can be equal, the flux d
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flux L will now decrease with incre
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this line is extrapolated to X = 0,
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since due to extinction, radiation
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96 5. Radiation Mechanisms Fig. 5.1
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98 5. Radiation Mechanisms From (5.
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100 5. Radiation Mechanisms Fig. 5.
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104 5. Radiation Mechanisms We now
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5. Radiation Mechanisms 106 Again F
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110 5. Radiation Mechanisms We can
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112 5. Radiation Mechanisms differe
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114 6. Celestial Mechanics The solu
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116 6. Celestial Mechanics prove (6
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118 6. Celestial Mechanics in the d
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120 6. Celestial Mechanics But cons
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122 6. Celestial Mechanics by the e
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124 6. Celestial Mechanics Substitu
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126 6. Celestial Mechanics a cloud
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128 6. Celestial Mechanics Since th
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130 6. Celestial Mechanics Exercise
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132 7. The Solar System Fig. 7.1. (
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134 7. The Solar System for each ob
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136 7. The Solar System Fig. 7.5. L
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138 7. The Solar System Inserting t
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140 7. The Solar System Therefore o
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142 7. The Solar System Fig. 7.10.
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144 7. The Solar System behaves mor
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146 7. The Solar System Table 7.1.
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150 7. The Solar System of the plan
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152 7. The Solar System If we denot
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154 7. The Solar System where F⊥
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158 7. The Solar System larized fea
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162 7. The Solar System The outer c
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168 7. The Solar System weak and co
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170 7. The Solar System amount of w
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176 7. The Solar System ter the rin
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178 7. The Solar System face, most
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180 7. The Solar System The F ring,
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182 7. The Solar System Herschel hi
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188 7. The Solar System liding, sin
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196 7. The Solar System of this mat
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202 7. The Solar System Near the po
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204 7. The Solar System be solved f
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8. Stellar Spectra All our informat
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which appears as irregular fluctuat
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8.2 The Harvard Spectral Classifica
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ate of ionization is essentially de
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lines of titanium, scandium and van
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efore τ = 1, i. e. the radiation i
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yielding Iν(0,θ)= Sν(τ ∗ ) +
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222 9. Binary Stars and Stellar Mas
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10. Stellar Structure The stars are
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where a = 4σ/c = 7.564 × 10−16
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where me is the electron mass and N
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is produced by the proton-proton (p
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oxygen, which in turn reacts to for
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According to (4.7), (4.4) and (5.16
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Example 10.6 The Radiation Pressure
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11. Stellar Evolution In the preced
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increases. The stellar surface temp
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Since stars are most likely to be f
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Fig. 11.4a-c. Energy transport in t
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Fig. 11.5. The structure of a massi
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tract to planetlike brown dwarfs. S
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Fig. 11.10a-f. Evolution of a low-m
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Fig. 11.12. The Wolf-Rayet star WR
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In a neutron capture, a nucleus wit
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This is several orders of magnitude
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264 12.TheSun Fig. 12.2. (a) The ro
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266 12.TheSun according to the heli
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268 12.TheSun shines into view for
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270 12.TheSun was established that
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272 12.TheSun Fig. 12.11. In pairs
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274 12.TheSun Fig. 12.15. (a) Quies
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276 12.TheSun Fig. 12.17. An X-ray
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13. Variable Stars Stars with chang
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Fig. 13.3. The variation of brightn
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Fig. 13.5. The lightcurve of a long
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duced when the carbon condenses int
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13.3 Eruptive Variables Fig. 13.12.
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Fig. 13.15. Supernova 1987A in the
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14. Compact Stars In astrophysics t
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about 1.4 M⊙, which is thus the u
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1968. In the following year it was
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ditions required for hypernova expl
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This is greater than the speed of l
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Fig. 14.12. Scale drawings of 16 bl
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are (or, in the radio case, have on
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14.6 Exercises Exercise 14.1 The ma
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308 15. The Interstellar Medium Fig
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310 15. The Interstellar Medium R d
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312 15. The Interstellar Medium pol
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318 15. The Interstellar Medium Tab
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322 15. The Interstellar Medium met
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324 15. The Interstellar Medium
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326 15. The Interstellar Medium He
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330 15. The Interstellar Medium up
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332 15. The Interstellar Medium hav
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334 15. The Interstellar Medium len
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336 15. The Interstellar Medium dro
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338 15. The Interstellar Medium the
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340 16. Star Clusters and Associati
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17. The Milky Way On clear, moonles
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Fig. 17.3. The directions to the ga
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classes of stars are main sequence
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Fig. 17.9. The size of the volume e
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lar material similarly moves in the
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Fig. 17.14. In order to derive Oort
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Fig. 17.17. The radial velocity as
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a suitable mass distribution, such
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esting because it may be a small-sc
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material constituting the galaxy. I
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18. Galaxies The galaxies are the f
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Fig. 18.3. The classification of no
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18.1 The Classification of Galaxies
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Fig. 18.7. Compound luminosity func
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In order to measure the mass at eve
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length r0 = 1-5 kpc. In Sc galaxies
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18.4 Dynamics of Galaxies We have s
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gas. Some normal spirals may have b
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the Large and Small Magellanic Clou
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stars are forming and evolving into
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panion galaxy. The tail is interpre
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een made at these wavelengths with
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galaxies in our present neighbourho
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394 19. Cosmology tographs form an
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396 19. Cosmology Fig. 19.3. Hubble
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398 19. Cosmology element after hyd
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400 19. Cosmology 19.3 Homogeneous
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402 19. Cosmology The potential ene
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404 19. Cosmology In an expanding c
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406 19. Cosmology about 40,000 degr
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408 19. Cosmology rather slowly. In
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410 19. Cosmology Fig. 19.15. Corre
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412 19. Cosmology where Ω0 = ρ0/
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414 19. Cosmology Example 19.2 Find
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416 20. Astrobiology According to t
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418 20. Astrobiology of spiral gala
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420 20. Astrobiology Fig. 20.2. Bla
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422 20. Astrobiology reached 10% of
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424 20. Astrobiology Now panspermia
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426 20. Astrobiology 20.9 Detecting
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428 20. Astrobiology cles that we s
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Appendices 431
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Ellipse. Equation in rectangular co
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A and B can be determined graphical
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When using matrix formalism it is c
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Similarly, a volume integral I = f
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B. Theory of Relativity Albert Eins
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time interval between the events is
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C. Tables Table C.1. SI basic units
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Table C.6. The Sun Property Symbol
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Table C.11. Osculating elements of
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Discoverer Year of a Psid e i r M
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Table C.16. Periodic comets with se
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Table C.17 (continued) C. Tables Na
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C. Tables Table C.19. Some double s
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Table C.22. Optically brightest gal
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Table C.23 (continued) Abbreviation
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C. Tables Table C.26. Millimetre an
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Table C.27 (continued) Satellite La
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468 Answers to Exercises 6.2 a = 1.
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470 Answers to Exercises Chapter 17
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472 Further Reading Morrison (ed.):
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474 Further Reading Maps and Catalo
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Name and Subject Index A aberration
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coherent radiation 95 Cold Dark Mat
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forbidden transition 101, 332 four-
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Kellman, Edith 212 Kepler’s equat
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nautical mile 15 nautical triangle
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Reber, Grote 69 recombination 95, 9
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synchronous rotation 135 synchrotro
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Colour Supplement 491
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Plate 14. The first view from the s
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Plate 1 Plate 2 Colour Supplement 4
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Plate 6 Plate 5 Colour Supplement 4
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Plate 9 Colour Supplement Plate 10
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Plate 23 Plate 24 Colour Supplement
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Colour Supplement Plate 29 507
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Fundamental Astronomy

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