Fundamental Astronomy

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

Table C.6. The Sun Property Symbol Numerical value Mass M⊙ 1.989 × 10 30 kg Radius R⊙ 6.960 × 10 8 m = 0.00465 AU Effective temperature Te 5785 K Luminosity L⊙ 3.9 × 10 26 W Apparent visual magnitude V −26.78 Colour indices B − V 0.62 U − B 0.10 Absolute visual magnitude MV 4.79 Absolute bolometric magnitude Mbol 4.72 Inclination of equator to ecliptic 7 ◦ 15 ′ Equatorial horizontal parallax π⊙ 8.794 ′′ Motion: direction of apex α = 270 ◦ δ = 30 ◦ velocity in LSR 19.7kms −1 Distance from galactic centre 8.5 kpc Table C.7. The Earth Property Symbol Numerical value Mass M⊕ = M⊙/332,946 = 5.974 × 10 24 kg Mass, Earth+Moon M⊕ + M ª = M⊙/328,900.5 = 6.048 × 10 24 kg Equatorial radius Re = 6,378,137 m Polar radius Rp = 6,356,752 m Flattening f = (Re − Rp)/Re = 1/298.257 Surface gravity g = 9.81 m s −2 Table C.8. The Moon Property Symbol Numerical value Mass M ª = M⊕/81.30 = 7.348 × 10 22 kg Radius R ª = 1738 km Surface gravity g ª = 1.62 m s −2 = 0.17 g Mean equatorial horizontal parallax π ª = 57 ′ Semimajor axis of the orbit a = 384,400 km Smallest distance from Earth rmin = 356,400 km Greatest distance from Earth rmax = 406,700 km Mean inclination of orbit to ecliptic ι = 5.145 ◦ C. Tables 447
448 C. Tables Table C.9. Planets. Re = equatorial radius, ρ = mean density, τsid = sidereal rotation period (R indicates retrograde rotation), ε = inclination of the equator with respect to the ecliptic (at the beginning of 2000), f = flattening, T = surface temperature, p = geometric albedo, V0 = mean opposition magnitude. The data are based mostly on the Astronomical Almanac Name Re Mass ρ Number of known planet planet + satellites satellites [km] [kg] [M⊕] [M⊙] [g/cm 3 ] Mercury 2,440 3.30 × 10 23 0.0553 1/6,023,600 5.4 – Venus 6,052 4.87 × 10 24 0.8150 1/408,523.5 5.2 – Earth 6,378 5.97 × 10 24 1.0123 1/328,900.5 5.5 1 Mars 3,397 6.42 × 10 23 0.1074 1/3,098,710 3.9 2 Jupiter 71,492 1.90 × 10 27 317.89 1/1,047.355 1.3 63 Saturn 60,268 5.69 × 10 26 95.17 1/3,498.5 0.7 56 Uranus 25,559 8.66 × 10 25 14.56 1/22,869 1.3 27 Neptune 24,764 1.03 × 10 26 17.24 1/19,314 1.8 13 Name τsid ε f T p V0 [deg] [K] Mercury 58.646 d 0.0 0 130–615 0.106 – Venus 243.019 d R 177.4 0 750 0.65 – Earth 23 h 56 min 04.1s 23.4 0.003353 300 0.367 – Mars 24 h 37 min 22.6s 25.2 0.006476 220 0.150 − 2.01 Jupiter 9 h 55 min 30 s 3.1 0.06487 140 0.52 − 2.70 Saturn 10 h 39 min 22 s 26.7 0.09796 100 0.47 + 0.67 Uranus 17 h 14 min 24 s R 97.8 0.02293 65 0.51 + 5.52 Neptune 16 h 06 min 36 s 28.3 0.01708 55 0.41 + 7.84 Table C.10. Magnitudes of the planets. The table gives the expressions used in the Astronomical Almanac. They give the magnitudes as functions of the phase angle α. Interior planets can be observed at relatively large phase angles, and thus several terms are needed to describe their phase curves. Phase angles of the exterior planets are always small, and thus very simple expressions are sufficient. The magnitude of Saturn means the magnitude of the planet only; the total magnitude also depends on the orientation of the rings V(1, 0) V(1,α) Mercury −0.36 V(1, 0) + 3.80(α/100 ◦ ) −2.73(α/100 ◦ ) 2 + 2.00(α/100 ◦ ) 3 Venus −4.29 V(1, 0) + 0.09(α/100 ◦ ) +2.39(α/100 ◦ ) 2 − 0.65(α/100 ◦ ) 3 Mars −1.52 V(1, 0) + 1.60(α/100 ◦ ) Jupiter −9.25 V(1, 0) + 0.5(α/100 ◦ ) Saturn −8.88 Uranus −7.19 V(1, 0) + 0.28(α/100 ◦ ) Neptune −6.87 V(1, 0)
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Fundamental Astronomy
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Dr. Hannu Karttunen University of T
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VI Preface to the First Edition The
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VIII Contents 5.6 Continuous Spectr
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X Contents 16. Star Clusters and As
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1. Introduction 1.1 TheRoleofAstron
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1.2 Astronomical Objects of Researc
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theory of relativity must be used t
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of the gas may be 10 −21 kg m −
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12 2. Spherical Astronomy angles co
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14 or 2. Spherical Astronomy sin B
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16 2. Spherical Astronomy defined t
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18 2. Spherical Astronomy the verna
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20 2. Spherical Astronomy pole. The
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22 2. Spherical Astronomy Fig. 2.16
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26 2. Spherical Astronomy
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30 2. Spherical Astronomy numbers,
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32 2. Spherical Astronomy In the 19
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34 2. Spherical Astronomy mid-Septe
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36 2. Spherical Astronomy correspon
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38 2. Spherical Astronomy second of
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2. Spherical Astronomy 40 Since ∆
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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
Page 396 and 397: 396 19. Cosmology Fig. 19.3. Hubble
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Page 400 and 401: 400 19. Cosmology 19.3 Homogeneous
Page 402 and 403: 402 19. Cosmology The potential ene
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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
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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 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
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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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