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3. The World of Galaxies 140 by no means isolated systems: their mass continuously changes through accretion <strong>and</strong> merging processes. In addition, the kinetic energy transferred to the ISM by supernova explosions causes an outflow of the ISM, in particular in low-mass galaxies where the gas is not strongly gravitationally bound. Therefore, the observed deviations from relation (3.72) allow us to draw conclusions about these processes. Also, from observations in our Milky Way we find indications that the model of the chemical evolution sketched above is too simplified. This is known as the G-dwarf problem. The model described above predicts that about half of the F- <strong>and</strong> G-main-sequence stars should have a metallicity of less than a quarter of the Solar value. These stars have a long lifetime on the main sequence, so that many of those observed today should have been formed in the early stages of the Galaxy. Thus, in accordance with our model they should have very low metallicity. However, a low metallicity is in fact observed in only very few of these stars. The discrepancy is far too large to be explained by selection effects. Rather, observations show that the chemical evolution of our Galaxy must have been substantially more complicated than described by our simple model.
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Peter Schneider Extragalactic Astro
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Prof. Dr. Peter Schneider Argelande
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Preface VI ter aspects are discusse
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List of Contents VIII 2.5.1 The Gra
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List of Contents X 5. Active Galact
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List of Contents XII 8. Cosmology I
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List of Contents XIV D. Recommended
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1. Introduction and Overview 2 Fig.
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1. Introduction and Overview 4 othe
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1. Introduction and Overview 6 obje
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1. Introduction and Overview 8 Fig.
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1. Introduction and Overview 10 Fig
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1. Introduction and Overview 16 of
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1. Introduction and Overview 18 app
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1. Introduction and Overview 26 spe
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2. The Milky Way as a Galaxy 35 The
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2.2 Determination of Distances With
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2.3 The Structure of the Galaxy Fig
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2.3 The Structure of the Galaxy a c
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2.3 The Structure of the Galaxy Fig
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2.3 The Structure of the Galaxy B-s
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2.3 The Structure of the Galaxy Fro
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2.3 The Structure of the Galaxy tha
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2.4 Kinematics of the Galaxy 57 2.4
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2.4 Kinematics of the Galaxy which
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2.4 Kinematics of the Galaxy where
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2.4 Kinematics of the Galaxy center
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2.5 The Galactic Microlensing Effec
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2.6 The Galactic Center have been e
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2.6 The Galactic Center 79 Fig. 2.3
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2.6 The Galactic Center Fig. 2.36.
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2.6 The Galactic Center 83 Fig. 2.3
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2.6 The Galactic Center hence, this
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3. The World of Galaxies 88 million
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3. The World of Galaxies 90 100M
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3. The World of Galaxies 92 Table 3
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3. The World of Galaxies 94 arrives
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96 3. The World of Galaxies This in
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3. The World of Galaxies 98 Boxines
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3. The World of Galaxies 100 Wherea
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3. The World of Galaxies 102 the po
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3. The World of Galaxies 104 The ki
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3. The World of Galaxies 106 Fig. 3
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3. The World of Galaxies 108 where
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3. The World of Galaxies 110 angula
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3. The World of Galaxies 112 Fig. 3
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Page 310: 4. Cosmology I: Homogeneous Isotrop
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4.4 Thermal History of the Universe
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4.4 Thermal History of the Universe
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4.5 Achievements and Problems of th
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5. Active Galactic Nuclei 175 The l
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5.1 Introduction 5.1 Introduction 5
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5.1 Introduction 179 Fig. 5.5. Radi
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5.1 Introduction The synchrotron sp
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5.2 AGN Zoology have in common stro
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5.3 The Central Engine: A Black Hol
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5.4 Components of an AGN 5.4 Compon
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5.4 Components of an AGN transition
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5.4 Components of an AGN Fig. 5.22.
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5.4 Components of an AGN by magneti
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5.4 Components of an AGN sible to o
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5.4 Components of an AGN ity of an
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5. Active Galactic Nuclei 208 radia
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5. Active Galactic Nuclei 210 Fig.
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5. Active Galactic Nuclei 212 5.5.4
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5. Active Galactic Nuclei 214 elect
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5. Active Galactic Nuclei 216 QSOs
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5. Active Galactic Nuclei 218 tion.
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5.6 AGNs and Cosmology 221 ize hydr
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6. Clusters and Groups of Galaxies
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6.1 The Local Group 225 Table 6.1.
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7. Cosmology II: Inhomogeneities in
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7.2 Gravitational Instability gravi
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7.2 Gravitational Instability i.e.,
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7.3 Description of Density Fluctuat
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7.4 Evolution of Density Fluctuatio
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7.4 Evolution of Density Fluctuatio
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7.5 Non-Linear Structure Evolution
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7.7 Origin of the Density Fluctuati
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8. Cosmology III: The Cosmological
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352 8. Cosmology III: The Cosmologi
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9. The Universe at High Redshift 35
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10. Outlook 407 In the final chapte
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10. Outlook telescope will start a
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10. Outlook New windows to the Univ
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10. Outlook understand why the dens
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Appendix
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A. The Electromagnetic Radiation Fi
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B. Properties of Stars 425 In this
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B.3 Structure and Evolution of Star
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B.3 Structure and Evolution of Star
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D. Recommended Literature 433 In th
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D.3 Review Articles, Current Litera
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E. Acronyms Used 438 GRB Gamma-Ray
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F. Figure Credits 441 Chapter 1 1.1
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F. Figure Credits 1.25 Source: R. W
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F. Figure Credits Nik Szymanek. bot
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F. Figure Credits 5.5 Credit: Laing
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F. Figure Credits 6.26 Source: http
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F. Figure Credits 8.24 Credit: Hu &
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Subject Index 453 A AB magnitudes 4
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Subject Index 455 Doppler effect 38
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Subject Index 457 -dampedLyα syste
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Subject Index 459 virial theorem 13
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