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E-grāmata: Essential Astrophysics

4.78/5 (18 ratings by Goodreads)
  • Formāts: PDF+DRM
  • Sērija : Undergraduate Lecture Notes in Physics
  • Izdošanas datums: 24-May-2013
  • Izdevniecība: Springer-Verlag Berlin and Heidelberg GmbH & Co. K
  • Valoda: eng
  • ISBN-13: 9783642359637
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Essential AstrophysicsPalielināt
  • Formāts: PDF+DRM
  • Sērija : Undergraduate Lecture Notes in Physics
  • Izdošanas datums: 24-May-2013
  • Izdevniecība: Springer-Verlag Berlin and Heidelberg GmbH & Co. K
  • Valoda: eng
  • ISBN-13: 9783642359637
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Essential Astrophysics is a book to learn or teach from, as well as a fundamental reference volume for anyone interested in astronomy and astrophysics. It presents astrophysics from basic principles without requiring any previous study of astronomy or astrophysics. It serves as a comprehensive introductory text, which takes the student through the field of astrophysics in lecture-sized chapters of basic physical principles applied to the cosmos.This one-semester overview will be enjoyed by undergraduate students with an interest in the physical sciences, such as astronomy, chemistry, engineering or physics, as well as by any curious student interested in learning about our celestial science. The mathematics required for understanding the text is on the level of simple algebra, for that is all that is needed to describe the fundamental principles. The text is of sufficient breadth and depth to prepare the interested student for more advanced specialized courses in the future. Astronomical examples are provided throughout the text, to reinforce the basic concepts and physics, and to demonstrate the use of the relevant formulae. In this way, the student learns to apply the fundamental equations and principles to cosmic objects and situations. All of the examples are solved with the rough accuracy needed to portray the basic result. Astronomical and physical constants and units as well as the most fundamental equations can be found in the appendix. Essential Astrophysics goes beyond the typical textbook by including references to the seminal papers in the field, with further reference to recent applications, results, or specialized literature. There are fifty set-aside focus elements that enhance and augment the discussion with fascinating details. They include the intriguing historical development of particular topics and provide further astrophysics equations or equations for other topics.Kenneth Lang is a world-renowned author on astrophysics. His books for professional astrophysicists as well as for students and the interested layman are highly acclaimed.

This book presents astrophysics from basic principles without requiring any previous study of astronomy or astrophysics. This one-semester overview provides 15 lecture-sized chapters and 50 set-aside focus elements.

Recenzijas

From the reviews:

This work fills a unique position in the literature. It is a concrete, middle-level treatment that devotes as much attention to methods of research and observation as it does to results. Here at last is a book in English which bridges the gap between elementary introductory accounts and advanced technical monographs. It is also a fine book for hobbyists and others with some grounding in astronomy who want to explore these matters in greater depth than elementary texts allow. (Philosophy, Religion and Science Book Reviews, bookinspections.wordpress.com, May, 2014)





This set of lecture notes on astrophysics discusses the topics that would be taught in an introductory undergraduate class. The text is sufficiently comprehensive to be used as the principle textbook for a lecture course or for self-study. the references are excellent, enabling those who need more detail to find information quickly. The book will be easy to follow for anyone witha solid background in lower-level undergraduate physics. A valuable acquisition for academic library collections. Summing Up: Highly recommended. Upper-division undergraduates and above. (A. Spero, Choice, Vol. 51 (6), February, 2014)

1 Observing the Universe 1(32)
1.1 What Do Astronomers and Astrophysicists Do?
1(1)
1.2 Our Place on Earth
2(2)
1.3 Location in the Sky
4(5)
1.4 Measuring Angle and Size
9(1)
1.5 The Locations of the Stars are Slowly Changing
10(5)
1.6 What Time is It?
15(2)
1.7 Telling Time by the Stars
17(2)
1.8 Optical Telescopes Observe Visible Light
19(4)
1.9 Telescopes that Detect Invisible Radiation
23(4)
1.10 Units Used by Astronomers and Astrophysicists
27(3)
1.11 Physical Constants
30(3)
2 Radiation 33(36)
2.1 Electromagnetic Waves
33(4)
2.2 The Electromagnetic Spectrum
37(3)
2.3 Moving Perspectives
40(4)
2.4 Thermal (Blackbody) Radiation
44(6)
2.5 How Far Away is the Sun, and How Bright, Big and Hot is it?
50(9)
2.5.1 Distance of the Sun
50(4)
2.5.2 How Big is the Sun?
54(1)
2.5.3 The-Unit of Energy
54(1)
2.5.4 The Sun's Luminosity
55(1)
2.5.5 Taking the Sun's Temperature
55(1)
2.5.6 How Hot are the Planets?
56(3)
2.6 The Energy of Light
59(2)
2.7 Radiation Scattering and Transfer
61(8)
2.7.1 Why is the Sky Blue and the Sunsets Red?
61(1)
2.7.2 Rayleigh Scattering
62(1)
2.7.3 Thomson and Compton Scattering
63(2)
2.7.4 Radiation Transfer
65(4)
3 Gravity 69(30)
3.1 Ceaseless, Repetitive Paths Across the Sky
69(4)
3.2 Universal Gravitational Attraction
73(7)
3.3 Mass of the Sun
80(1)
3.4 Tidal Effects
81(12)
3.4.1 The Ocean Tides
81(4)
3.4.2 Tidal Locking into Synchronous Rotation
85(1)
3.4.3 The Days are Getting Longer
85(2)
3.4.4 The Moon is Moving Away from the Earth
87(3)
3.4.5 A Planet's Differential Gravitational Attraction Accounts for Planetary Rings
90(3)
3.5 What Causes Gravity?
93(6)
4 Cosmic Motion 99(26)
4.1 Motion Opposes Gravity
99(2)
4.1.1 Everything Moves
99(1)
4.1.2 Escape Speed
99(2)
4.2 Orbital Motion
101(4)
4.3 The Moving Stars
105(11)
4.3.1 Are the Stars Moving?
105(1)
4.3.2 Components of Stellar Velocity
105(2)
4.3.3 Proper Motion
107(1)
4.3.4 Radial Velocity
107(2)
4.3.5 Observed Proper Motions of Stars
109(2)
4.3.6 Motions in Star Clusters
111(3)
4.3.7 Runaway Stars
114(2)
4.4 Cosmic Rotation
116(9)
4.4.1 Unexpected Planetary Rotation
116(4)
4.4.2 The Sun's Differential Rotation
120(4)
4.4.3 Stellar Rotation and Age
124(1)
5 Moving Particles 125(34)
5.1 Elementary Constituents of Matter
125(5)
5.2 Heat, Temperature, and Speed
130(8)
5.2.1 Where Does Heat Come From?
130(2)
5.2.2 Thermal Velocity
132(2)
5.2.3 Collisions
134(1)
5.2.4 The Distribution of Speeds
135(3)
5.3 Molecules in Planetary Atmospheres
138(3)
5.4 Gas Pressure
141(8)
5.4.1 What Keeps Our Atmosphere Up?
141(1)
5.4.2 The Ideal Gas Law
142(2)
5.4.3 The Earth's Sun-Layered Atmosphere
144(4)
5.4.4 Pressure, Temperature, and Density Inside the Sun
148(1)
5.5 Plasma
149(5)
5.5.1 Ionized Gas
149(3)
5.5.2 Plasma Oscillations and the Plasma Frequency
152(1)
5.5.3 Atoms are Tom Apart into Plasma Within the Sun
153(1)
5.6 Sound Waves and Magnetic Waves
154(5)
5.6.1 Sound Waves
154(2)
5.6.2 Magnetic Waves
156(3)
6 Detecting Atoms in Stars 159(32)
6.1 What is the Sun Made Out Of?
159(6)
6.2 Quantization of Atomic Systems
165(8)
6.3 Some Atoms are Excited Out of Their Lowest-Energy Ground State
173(3)
6.4 Ionization and Element Abundance in the Sun and Other Stars
176(4)
6.5 Wavelengths and Shapes of Spectral Lines
180(11)
6.5.1 Radial Motion Produces a Wavelength Shift
180(1)
6.5.2 Gravitational Redshift
181(2)
6.5.3 Thermal Motion Broadens Spectral Lines
183(1)
6.5.4 Rotation or Expansion of the Radiating Source can Broaden Spectral Lines
184(1)
6.5.5 Curve of Growth
185(1)
6.5.6 Magnetic Fields Split Spectral Lines
186(5)
7 Transmutation of the Elements 191(24)
7.1 The Electron, X-rays and Radium
191(2)
7.2 Radioactivity
193(3)
7.3 Tunneling Out of the Atomic Nucleus
196(3)
7.4 The Electron and the Neutrino
199(3)
7.5 Cosmic Rays
202(7)
7.6 Nuclear Transformation by Bombardment
209(6)
8 What Makes the Sin Shine? 215(40)
8.1 Can Gravitational Contraction Supply the Sun's Luminosity?
215(2)
8.2 How Hot is the Center of the Sun?
217(2)
8.3 Nuclear Fusion Reactions in the Sun's Core
219(18)
8.3.1 Mass Lost is Energy Gained
219(6)
8.3.2 Understanding Thermonuclear Reactions
225(6)
8.3.3 Hydrogen Burning
231(6)
8.3.4 Why Doesn't the Sun Blow Up?
237(1)
8.4 The Mystery of Solar Neutrinos
237(7)
8.4.1 The Elusive Neutrino
237(2)
8.4.2 Solar Neutrino Detectors Buried Deep Underground
239(3)
8.4.3 Solving the Solar Neutrino Problem
242(2)
8.5 How the Energy Gets Out
244(8)
8.6 The Faint-Young-Sun Paradox
252(1)
8.7 The Sun's Destiny
253(2)
9 The Extended Solar Atmosphere 255(38)
9.1 Hot, Volatile, Magnetized Gas
255(13)
9.1.1 The Million-Degree Solar Corona
255(3)
9.1.2 Varying Sunspots and Ever-Changing Magnetic Fields
258(3)
9.1.3 Coronal Loops
261(5)
9.1.4 What Heats the Corona?
266(2)
9.1.5 Coronal Holes
268(1)
9.2 The Sun's Varying Winds
268(8)
9.2.1 The Expanding Sun Envelops the Earth
268(3)
9.2.2 Properties of the Solar Wind
271(3)
9.2.3 Where Do the Two Solar Winds Come From?
274(1)
9.2.4 Where Does the Solar Wind End?
275(1)
9.3 Explosions on the Sun
276(7)
9.3.1 Solar Flares
276(5)
9.3.2 Coronal Mass Ejections
281(2)
9.4 Space Weather
283(10)
9.4.1 Earth's Protective Magnetosphere
283(4)
9.4.2 Trapped Particles
287(1)
9.4.3 Earth's Magnetic Storms
288(1)
9.4.4 Solar Explosions Threaten Humans in Outer Space
289(1)
9.4.5 Disrupting Communication
290(1)
9.4.6 Satellites in Danger
291(1)
9.4.7 Forecasting Space Weather
292(1)
10 The Sun Amongst the Stars 293(64)
10.1 Comparisons of the Sun with Other Stars
293(25)
10.1.1 How Far Away are the Stars?
293(3)
10.1.2 How Bright are the Stars?
296(2)
10.1.3 How Luminous are the Stars?
298(5)
10.1.4 The Temperatures of Stars
303(1)
10.1.5 The Colors of Stars
304(1)
10.1.6 The Spectral Sequence
305(1)
10.1.7 Radius of the Stars
306(4)
10.1.8 How Massive are the Stars?
310(8)
10.2 Main-Sequence and Giant Stars
318(11)
10.2.1 The Hertzsprung-Russell Diagram
318(3)
10.2.2 The Luminosity Class
321(2)
10.2.3 Life on the Main Sequence
323(3)
10.2.4 The Red Giants and Supergiants
326(3)
10.3 Nuclear Reactions Inside Stars
329(14)
10.3.1 The Internal Constitution of Stars
329(6)
10.3.2 Two Ways to Bum Hydrogen in Main-Sequence Stars
335(5)
10.3.3 Helium Burning in Giant Stars
340(3)
10.4 Using Star Clusters to Watch How Stars Evolve
343(5)
10.5 Where did the Chemical Elements Come From?
348(9)
10.5.1 Advanced Nuclear Burning Stages in Massive Supergiant Stars
348(1)
10.5.2 Origin of the Material World
349(1)
10.5.3 The Observed Abundance of the Elements
350(1)
10.5.4 Synthesis of the Elements Inside Stars
351(2)
10.5.5 Big-Bang Nucleosynthesis
353(1)
10.5.6 The First and Second Generation of Stars
354(1)
10.5.7 Cosmic Implications of the Origin of the Elements
355(2)
11 The Material Between the Stars 357(24)
11.1 Gaseous Emission Nebulae
357(9)
11.2 Solid Dust Particles in Interstellar Space
366(3)
11.3 Radio Emission from the Milky Way
369(6)
11.4 Interstellar Hydrogen Atoms
375(3)
11.5 Interstellar Molecules
378(3)
12 Formation of the Stars and Their Planets 381(30)
12.1 How the Solar System Came into Being
381(7)
12.1.1 The Nebular Hypothesis
381(1)
12.1.2 Composition of the Planets
382(3)
12.1.3 Mass and Angular Momentum in the Solar System
385(3)
12.2 Star Formation
388(12)
12.2.1 Giant Molecular Clouds
388(1)
12.2.2 Gravitational Collapse
389(3)
12.2.3 Triggering Gravitational Collapse
392(3)
12.2.4 Protostars
395(3)
12.2.5 Losing Mass and Spin
398(2)
12.3 Planet-Forming Disks and Planets Around Nearby Stars
400(11)
12.3.1 The Plurality of Worlds
400(1)
12.3.2 Proto-Planetary Disks
400(3)
12.3.3 The First Discoveries of Exoplanets
403(5)
12.3.4 Hundreds of New Worlds Circling Nearby Stars
408(1)
12.3.5 Searching for Habitable Planets
409(2)
13 Stellar End States 411(60)
13.1 A Range of Destinies
411(1)
13.2 Planetary Nebulae
412(6)
13.3 Stars the Size of the Earth
418(5)
13.3.1 The Discovery of White Dwarf Stars
418(1)
13.3.2 Unveiling White Dwarf Stars
419(1)
13.3.3 The High Mass Density of White Dwarf Stars
420(3)
13.4 The Degenerate Electron Gas
423(6)
13.4.1 Nuclei Pull a White Dwarf Together as Electrons Support It
423(4)
13.4.2 Radius and Mass of a White Dwarf
427(2)
13.5 Exploding Stars
429(14)
13.5.1 Guest Stars, the Novae
429(1)
13.5.2 What Makes a Nova Happen'?
430(3)
13.5.3 A Rare and Violent End, the Supernovae
433(3)
13.5.4 Why do Supernova Explosions Occur?
436(1)
13.5.5 When a Nearby Star Detonates Its Companion
437(1)
13.5.6 Stars that Blow Themselves Up
438(1)
13.5.7 Light of a Billion Suns, SN 1987A
439(4)
13.5.8 Will the Sun Explode?
443(1)
13.6 Expanding Stellar Remnants
443(7)
13.7 Neutron Stars and Pulsars
450(15)
13.7.1 Neutron Stars
450(3)
13.7.2 Radio Pulsars from Isolated Neutron Stars
453(7)
13.7.3 X-ray Pulsars from Neutron Stars in Binary Star Systems
460(5)
13.8 Stellar Black Holes
465(6)
13.8.1 Imagining Black Holes
465(1)
13.8.2 Observing Stellar Black Holes
466(1)
13.8.3 Describing Black Holes
467(4)
14 A Larger, Expanding Universe 471(52)
14.1 The Milky Way
471(16)
14.1.1 A Fathomless Disk of Stars
471(2)
14.1.2 The Sun is Not at the Center of Our Stellar System
473(6)
14.1.3 The Rotating Galactic Disk
479(3)
14.1.4 Whirling Coils of the Milky Way
482(2)
14.1.5 A Central Super-Massive Black Hole
484(2)
14.1.6 Dark Matter Envelops the Milky Way
486(1)
14.2 The Discovery of Galaxies
487(4)
14.3 The Galaxies are Moving Away from us and from Each Other
491(9)
14.4 Galaxies Gather and Stream Together
500(12)
14.4.1 Clusters of Galaxies
500(2)
14.4.2 Dark Matter in Clusters of Galaxies
502(6)
14.4.3 Cosmic Streams
508(2)
14.4.4 Galaxy Walls and Voids
510(2)
14.5 Looking Back into Time
512(5)
14.6 Using Einstein's General Theory of Relativity to Explain the Expansion
517(6)
15 Origin, Evolution, and Destiny of the Observable Universe 523(38)
15.1 Hotter Than Anything Else
523(3)
15.2 Three Degrees Above Absolute Zero
526(6)
15.2.1 An Unexpected Source of Noise
526(1)
15.2.2 Blackbody Spectrum
527(2)
15.2.3 As Smooth as Silk
529(1)
15.2.4 Cosmic Ripples
529(3)
15.3 The Beginning of the Material Universe
532(9)
15.3.1 The First Three Minutes
532(3)
15.3.2 Formation of the First Atoms, and the Amount of Invisible Dark Matter
535(2)
15.3.3 History of the Expanding Universe
537(4)
15.4 The First Stars and Galaxies
541(4)
15.4.1 Pulling Primordial Material Together
541(1)
15.4.2 When Stars Began to Shine
542(3)
15.5 The Evolution of Galaxies
545(9)
15.5.1 Active Galactic Nuclei
545(5)
15.5.2 Super-Massive Black Holes
550(2)
15.5.3 Gamma-Ray Bursts
552(2)
15.6 Dark Energy, the Cosmological Constant, and How it All Ends
554(7)
15.6.1 Discovery of Dark Energy
554(1)
15.6.2 Using the Cosmological Constant to Describe Dark Energy
555(5)
15.6.3 When Stars Cease to Shine
560(1)
16 References 561(46)
Appendix I: Constants 607(2)
Appendix II: Units 609(2)
Appendix III: Fundamental Equations 611(4)
Author Index 615(4)
Subject Index 619
Kenneth R. Lang is professor in the Astronomy and Astrophysics group at Tufts University, Medford, MA, USA. He is the author of several successful books (textbooks and popular science books) including "Astrophysical Formulae", "The Sun from Space" or "Parting the Cosmic Veil".
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