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  • ISBN-10 ‏ : ‎ 1464181705
  • ISBN-13 ‏ : ‎ 978-1464181702
  • Author:   Neil F. Comins

Neil Comins’ Discovering the Universe confronts the challenges of the one-term astronomy course by heightening student curiosities about the cosmos, by using the context of astronomy to teach the process of science, and by highlighting common misconceptions and showing students how to think their way past them. With its signature combination of vivid writing and spectacular images, the new edition offers new findings, new study help, and an expanded new media/supplements package centered on W.H. Freeman’s breakthrough online course space, LaunchPad.

 

Table of Content:

  1. CHAPTER 1 Discovering the Night Sky
  2. NAVIGATING THE NIGHT SKY
  3. 1-1 The night sky is full of patterns
  4. 1-2 Constellations make locating stars easy
  5. 1-3 The celestial sphere aids in navigating the sky
  6. 1-4 An “alt”ernative coordinate system
  7. 1-5 Earth orbits the Sun in a plane called the ecliptic
  8. EARTHLY CYCLES
  9. 1-6 Earth’s rotation creates the day-night cycle and its revolution defines a year
  10. THE SEASONS
  11. 1-7 The seasons result from the tilt of Earth’s rotation axis combined with Earth’s revolution aroun
  12. 1-8 Clocks and calendars are based on Earth’s rotation and revolution
  13. 1-9 Precession is a slow, circular motion of Earth’s axis of rotation
  14. THE PHASES OF THE MOON
  15. 1-10 The phases of the Moon originally inspired the concept of the month
  16. ECLIPSES
  17. 1-11 Eclipses do not occur during every new or full Moon phase
  18. 1-12 Three types of lunar eclipses occur
  19. 1-13 Three types of solar eclipses also occur
  20. SCALES OF THE UNIVERSE
  21. 1-14 Astronomical distances are, well, astronomical
  22. Summary of Key Ideas
  23. CHAPTER 2 Gravitation and the Motion of the Planets
  24. SCIENCE: KEY TO COMPREHENDING THE COSMOS
  25. 2-1 Science is both a body of knowledge and a process of learning about nature
  26. CHANGING OUR EARTH-CENTERED VIEW OF THE UNIVERSE
  27. 2-2 The belief in a Sun-centered cosmology formed slowly
  28. DISCOVERY 2-1 Earth-Centered Universe
  29. 2-3 Copernicus devised the first comprehensive heliocentric cosmology
  30. 2-4 Tycho Brahe made astronomical observations that disproved ancient ideas about the heavens
  31. KEPLER’S AND NEWTON’S LAWS
  32. 2-5 Kepler’s laws describe orbital shapes, changing speeds, and the lengths of planetary years
  33. DISCOVERY 2-2 Units of Astronomical Distance
  34. 2-6 Galileo’s discoveries strongly supported a heliocentric cosmology
  35. 2-7 Newton formulated three laws that describe fundamental properties of physical reality
  36. 2-8 Newton’s description of gravity accounts for Kepler’s laws
  37. Summary of Key Ideas
  38. CHAPTER 3 Light and Telescopes
  39. THE NATURE OF LIGHT
  40. 3-1 Newton discovered that white is not a fundamental color and proposed that light is composed of p
  41. 3-2 Light travels at a finite but incredibly fast speed
  42. 3-3 Einstein showed that light sometimes behaves as particles that carry energy
  43. 3-4 Visible light is only one type of electromagnetic radiation
  44. OPTICS AND TELESCOPES
  45. 3-5 Reflecting telescopes use mirrors to concentrate incoming starlight
  46. 3-6 Telescopes brighten, resolve, and magnify
  47. 3-7 Eyepieces, refracting telescopes, and binoculars use lenses to focus incoming light
  48. 3-8 Shaping telescope mirrors and lenses is an evolving science
  49. 3-9 Storing and analyzing light from space is key to understanding the cosmos
  50. 3-10 Earth’s atmosphere hinders astronomical research
  51. CAPTURING NONVISIBLE LIGHT: NONOPTICAL ASTRONOMY
  52. 3-11 Specially designed telescopes gather electromagnetic energy in all of the nonvisible parts of t
  53. BLACKBODY RADIATION
  54. 3-12 An object’s peak color shifts to shorter wavelengths as it is heated
  55. 3-13 The relative intensities of different emitted colors reveal a star’s surface temperature
  56. IDENTIFYING THE ELEMENTS BY ANALYZING THEIR UNIQUE SPECTRA
  57. 3-14 Each chemical element produces its own unique set of spectral lines
  58. 3-15 The various brightness levels of spectral lines depend on conditions in the spectrum’s source
  59. ATOMS AND SPECTRA
  60. 3-16 An atom consists of a small, dense nucleus surrounded by electrons
  61. 3-17 Spectra occur because electrons absorb and emit photons with only certain wavelengths
  62. 3-18 Spectra provide information about motion of objects toward or away from us but not across the s
  63. Summary of Key Ideas
  64. CHAPTER 4 Formation of the Solar System
  65. THE SOLAR SYSTEM CONTAINS HEAVY ELEMENTS, FORMED FROM AN EARLIER GENERATION OF STARS
  66. 4-1 Stars transform matter from lighter elements into heavier ones
  67. 4-2 Gravity, rotation, collisions, and heat shaped the young solar system
  68. THE FORMATION OF THE PLANETS
  69. 4-3 The giant planets formed in sequence
  70. 4-4 The inner planets formed primarily from collisions
  71. DEBRIS: REMNANTS IN THE SOLAR SYSTEM
  72. 4-5 The changing orbits of the giant planets spread debris throughout the solar system
  73. 4-6 The asteroid belt is leftover debris
  74. 4-7 The infalling debris from the giant planets led to the Late Heavy Bombardment
  75. CATEGORIES OF THE PRESENT-DAY SOLAR SYSTEM
  76. 4-8 The categories of solar system objects have evolved
  77. 4-9 The orbits of the planets are related
  78. 4-10 The Sun developed while the planets matured
  79. Summary of Key Ideas
  80. CHAPTER 5 Exoplanets
  81. EXOPLANETS—PLANETS OUTSIDE OUR SOLAR SYSTEM
  82. 5-1 Protoplanetary disks are a common part of the star-forming process
  83. 5-2 Astronomers have at least seven different ways of detecting planets outside our solar system
  84. 5-3 Exoplanets orbit a breathtaking variety of stars
  85. 5-4 Exoplanets with a wide range of sizes, masses, and compositions have been observed
  86. 5-5 Stars with multiple planets have been observed
  87. 5-6 Many exoplanets have extraordinary orbits, as compared to those in our solar system
  88. 5-7 Planets that are not orbiting stars have also been observed
  89. 5-8 There are billions and billions of planets
  90. 5-9 Planets with liquid water are being discovered
  91. 5-10 The search for life on exoplanets is under way
  92. Summary of Key Ideas
  93. CHAPTER 6 The Terrestrial Planets and Their Moons
  94. COMPARATIVE PLANETOLOGY
  95. 6-1 Comparisons of the eight planets show distinct similarities and significant differences
  96. EARTH: A DYNAMIC, VITAL WORLD
  97. 6-2 Earth’s atmosphere has evolved over billions of years
  98. 6-3 Plate tectonics produce major changes on Earth’s surface
  99. 6-4 Earth’s interior consists of a rocky mantle and an iron-rich core
  100. 6-5 Earth’s magnetic field shields us from the solar wind
  101. THE MOON AND TIDES
  102. 6-6 The Moon’s surface is covered with craters, plains, and mountains
  103. 6-7 Visits to the Moon yielded invaluable information about its history
  104. 6-8 The Moon probably formed from debris cast into space when a huge planetesimal struck the young E
  105. 6-9 Tides have played several important roles in the history of Earth and the Moon
  106. 6-10 The Moon is moving away from Earth
  107. MERCURY
  108. 6-11 Photographs from Mariner 10 and Messenger spacecraft reveal Mercury’s lunarlike surface
  109. 6-12 Mercury has a higher percentage of iron than Earth
  110. 6-13 Mercury’s rotation and revolution are coupled
  111. 6-14 Mercury’s atmosphere is the thinnest of all terrestrial planets
  112. VENUS
  113. 6-15 The surface of Venus is completely hidden beneath a permanent cloud cover
  114. 6-16 The greenhouse effect heats Venus’s surface
  115. 6-17 Venus is covered with gently rolling hills, two “continents,” and numerous volcanoes
  116. MARS
  117. 6-18 Mars’s global features include plains, canyons, craters, and volcanoes
  118. 6-19 Although no canals exist on Mars, it does have some curious natural features
  119. 6-20 Mars’s interior is less molten than the inside of Earth
  120. 6-21 Martian air is thin and often filled with dust
  121. 6-22 Surface and underground features indicate that water once flowed on Mars
  122. 6-23 Search for microscopic life on Mars continues
  123. 6-24 Mars’s two moons look more like potatoes than spheres
  124. COMPARATIVE PLANETOLOGY OF THE INNER PLANETS
  125. 6-25 Comparisons of planetary features provide new insights
  126. Summary of Key Ideas
  127. CHAPTER 7 The Outer Planets and Their Moons
  128. JUPITER
  129. 7-1 Jupiter’s outer layer is a dynamic area of storms and turbulent gases
  130. 7-2 Jupiter’s interior has four distinct regions
  131. 7-3 Impacts provide probes into Jupiter’s atmosphere
  132. JUPITER’S MOONS AND RINGS
  133. 7-4 Io’s surface is sculpted by volcanic activity
  134. 7-5 Europa harbors liquid water below its surface
  135. 7-6 Ganymede is larger than Mercury
  136. 7-7 Callisto bears the scars of a huge asteroid impact
  137. 7-8 Other debris orbits Jupiter as smaller moons and ringlets
  138. SATURN
  139. 7-9 Saturn’s atmosphere, surface, and interior are similar to Jupiter
  140. 7-10 Saturn’s spectacular rings are composed of fragments of ice and ice-coated rock
  141. 7-11 Titan has a thick atmosphere, clouds, and lakes filled with liquids
  142. 7-12 Rhea has ice
  143. 7-13 Enceladus has water jets, an atmosphere, and a magnetic field
  144. URANUS
  145. 7-14 Uranus sports a hazy atmosphere and clouds
  146. 7-15 A system of rings and satellites revolves around Uranus
  147. NEPTUNE
  148. 7-16 Neptune was discovered because it had to be there
  149. 7-17 Neptune has rings and captured moons
  150. COMPARATIVE PLANETOLOGY OF THE OUTER PLANETS
  151. Summary of Key Ideas
  152. CHAPTER 8 Vagabonds of the Solar System
  153. DWARF PLANETS
  154. 8-1 Pluto and its moon, Charon, are about the same size
  155. 8-2 Ceres is a dwarf planet in the asteroid belt, while Pluto, Eris, Haumea, and Makemake are trans-
  156. SMALL SOLAR SYSTEM BODIES
  157. ASTEROIDS
  158. 8-3 Most asteroids orbit the Sun between Mars and Jupiter
  159. 8-4 Jupiter’s gravity creates gaps in the asteroid belt
  160. 8-5 Asteroids also orbit outside the asteroid belt
  161. COMETS
  162. 8-6 Comets come from far out in the solar system
  163. 8-7 Comet tails develop from gases and dust pushed outward by the Sun
  164. 8-8 Comets are fragile yet durable
  165. 8-9 Comets do not last forever
  166. METEOROIDS, METEORS, AND METEORITES
  167. 8-10 Small, rocky debris peppers the solar system
  168. 8-11 Meteorites are space debris that land intact
  169. 8-12 The Allende meteorite provides evidence of catastrophic explosions
  170. 8-13 Asteroid impacts with Earth have caused mass extinctions
  171. Summary of Key Ideas
  172. CHAPTER 9 The Sun: Our Extraordinary Ordinary Star
  173. THE SUN’S ATMOSPHERE
  174. 9-1 The photosphere is the visible layer of the Sun
  175. 9-2 The chromosphere is characterized by spikes of gas called spicules
  176. 9-3 The outermost layer of the Sun’s atmosphere, the corona, is exceptionally hot
  177. THE ACTIVE SUN
  178. 9-4 Sunspots reveal the solar cycle and the Sun’s rotation
  179. 9-5 The Sun’s magnetic fields create sunspots
  180. 9-6 Solar magnetic fields also create other atmospheric phenomena
  181. THE SUN’S INTERIOR
  182. 9-7 Thermonuclear reactions in the core of the Sun produce its energy
  183. 9-8 The solar model describes how energy escapes from the Sun’s core
  184. DISCOVERY 9-1 T hermonuclear Fusion
  185. 9-9 The Sun has gotten brighter over time
  186. 9-10 The mystery of the missing neutrinos inspired research into the fundamental nature of matter
  187. Summary of Key Ideas
  188. CHAPTER 10 Characterizing Stars
  189. LEAVING THE SOLAR SYSTEM
  190. 10-1 Distances to nearby stars are found using stellar parallax
  191. DISCOVERY 10-1 Distances to Nearby Stars
  192. MAGNITUDE SCALES
  193. 10-2 Apparent magnitude measures the brightness of stars as seen from Earth
  194. 10-3 Absolute magnitudes and luminosities do not depend on distance
  195. DISCOVERY 10-2 T he Distance–Magnitude Relationship
  196. THE TEMPERATURES OF STARS
  197. 10-4 A star’s color reveals its surface temperature
  198. 10-5 A star’s spectrum also reveals its surface temperature
  199. 10-6 Stars are classified by their spectra
  200. TYPES OF STARS
  201. 10-7 The Hertzsprung-Russell diagram identifies distinct groups of stars
  202. 10-8 Luminosity classes set the stage for understanding stellar evolution
  203. 10-9 A star’s spectral type and luminosity class provide a second distance-measuring technique
  204. DISCOVERY 10-3 Kepler’s Third Law and Stellar Masses
  205. STELLAR MASSES
  206. 10-10 Binary stars provide information about stellar masses
  207. 10-11 Main-sequence stars have a relationship between mass and luminosity
  208. 10-12 The orbital motion of binary stars affects the wavelengths of their spectral lines
  209. Summary of Key Ideas
  210. CHAPTER 11 The Lives of Stars from Birth Through Middle Age
  211. PROTOSTARS AND PRE–MAIN-SEQUENCE STARS
  212. 11-1 Gas and dust exist between the stars
  213. 11-2 Supernovae, collisions of interstellar clouds, and starlight trigger new star formation
  214. 11-3 When a protostar ceases to accumulate mass, it becomes a pre–main-sequence star
  215. 11-4 The evolutionary track of a pre–main-sequence star depends on its mass
  216. 11-5 H II regions harbor young star clusters
  217. 11-6 Plotting a star cluster on an H-R diagram reveals its age
  218. MAIN-SEQUENCE AND GIANT STARS
  219. 11-7 Stars spend most of their lives on the main sequence
  220. EVOLUTION OF LOW MASS (0.08–0.4 M(Omitted)) STARS
  221. 11-8 Red dwarfs convert essentially their entire mass into helium
  222. EARLY AND MIDDLE EVOLUTION OF INTERMEDIATE (0.4–8 M(Omitted)) AND HIGH-MASS STARS
  223. 11-9 When core hydrogen fusion slows down, a main-sequence star with mass greater than 0.4 M(Omitted
  224. 11-10 Helium fusion begins at the center of a giant
  225. 11-11 Life in the giant phase has its ups and downs
  226. VARIABLE STARS
  227. 11-12 A Cepheid pulsates because it is alternately expanding and contracting
  228. 11-13 Cepheids enable astronomers to estimate vast distances
  229. 11-14 Globular clusters are bound groups of old stars
  230. 11-15 Mass transfer in close binary systems can produce unusual double stars
  231. Summary of Key Ideas
  232. CHAPTER 12 The Deaths and Remnants of Stars
  233. INTERMEDIATE-MASS (0.4 M(Omitted)–8 M(Omitted)) STARS AND PLANETARY NEBULAE
  234. 12-1 Intermediate-mass stars become supergiants before expanding into planetary nebulae
  235. 12-2 The burned-out core of an intermediate-mass star becomes a white dwarf
  236. HIGH-MASS STARS (GREATER THAN 8 M(Omitted)) AND TYPE II SUPERNOVAE
  237. 12-3 A series of fusion reactions in high-mass stars leads to luminous supergiants
  238. 12-4 High-mass stars blow apart in Type II supernova explosions
  239. 12-5 Supernova remnants are observed in many places
  240. NEUTRON STARS AND PULSARS
  241. 12-6 The cores of many Type II supernovae become neutron stars
  242. 12-7 A rotating magnetic field explains the pulses from a neutron star
  243. 12-8 Neutron stars have internal structure
  244. 12-9 Colliding neutron stars may provide some of the heavy elements in the universe
  245. 12-10 Binary neutron stars create pulsating X-ray sources
  246. THE RELATIVITY THEORIES
  247. 12-11 Einstein revolutionized our understanding of space, time, and gravity
  248. INSIDE A BLACK HOLE
  249. 12-12 Matter in a black hole becomes much simpler than elsewhere in the universe
  250. 12-13 Falling into a black hole is an infinite voyage
  251. EVIDENCE FOR BLACK HOLES
  252. 12-14 Several binary star systems contain black holes
  253. 12-15 Other black holes range in mass up to billions of solar masses
  254. 12-16 Black holes and neutron stars in binary systems often create jets of gas
  255. GAMMA-RAY BURSTS
  256. 12-17 Gamma-ray bursts are the most powerful explosions in the known universe
  257. 12-18 Black holes evaporate
  258. Summary of Key Ideas
  259. CHAPTER 13 The Galaxies
  260. THE MILKY WAY
  261. 13-1 Studies of Cepheid variable stars revealed that the Milky Way is only one of many galaxies
  262. 13-2 Cepheid variables help us locate our Galaxy’s center
  263. 13-3 Nonvisible observations help map the galactic disk
  264. 13-4 The galactic nucleus is an active, crowded place
  265. 13-5 Our Galaxy’s disk is surrounded by a two-shell spherical halo of stars and other matter
  266. 13-6 The Galaxy is rotating
  267. MYSTERIES AT THE GALACTIC FRINGES
  268. 13-7 Most of the matter in the Galaxy has not yet been identified
  269. TYPES OF GALAXIES
  270. 13-8 The winding of a spiral galaxy’s arms is correlated to the size of its central bulge
  271. 13-9 Explosions create flocculent spirals, and waves create grand-design spirals
  272. 13-10 Bars of stars run through the central bulges of barred spiral galaxies, and some disk galaxies
  273. 13-11 Elliptical galaxies display a wide variety of sizes and masses
  274. 13-12 Galaxies without global structure are called irregular
  275. 13-13 Hubble presented spiral and elliptical galaxies in a tuning fork–shaped diagram
  276. CLUSTERS AND SUPERCLUSTERS
  277. 13-14 Galaxies exist in clusters that may form still larger clumps called superclusters
  278. 13-15 Galaxies in a cluster can collide and combine
  279. 13-16 Dark matter helps hold together individual galaxies and clusters of galaxies
  280. SUPERCLUSTERS IN MOTION
  281. 13-17 The redshifts of superclusters indicate that the universe is indeed expanding
  282. DISCOVERY 13-1 The Tully–Fisher Relation and Other Distance-Measuring Techniques
  283. DISCOVERY 13-2 The Expanding Universe
  284. 13-18 Astronomers are looking back to a time when galaxies were first forming
  285. QUASARS
  286. 13-19 Quasars look like stars but have huge redshifts
  287. OTHER ACTIVE GALAXIES
  288. 13-20 Active galaxies can be either spiral or elliptical
  289. SUPERMASSIVE ENGINES
  290. 13-21 Supermassive black holes exist at the centers of most galaxies
  291. 13-22 Jets of protons and electrons ejected from around black holes help explain active galaxies
  292. 13-23 Gravity focuses light from quasars
  293. Summary of Key Ideas
  294. CHAPTER 14 Cosmology
  295. COSMOLOGY
  296. 14-1 General relativity predicts an expanding (or contracting) universe
  297. 14-2 The expansion of the universe creates a Dopplerlike redshift
  298. 14-3 The Hubble constant is related to the age of the universe
  299. THE BIG BANG
  300. 14-4 Remnants of the Big Bang have been detected
  301. 14-5 The universe has two symmetries—isotropy and homogeneity
  302. A BRIEF HISTORY OF SPACETIME, MATTER, ENERGY, AND EVERYTHING
  303. 14-6 All physical forces in nature were initially unified
  304. 14-7 Equations explain the evolution of the universe, even before matter and energy, as we know them
  305. 14-8 Homogeneity and isotropy are results of inflation
  306. 14-9 During the first second, most of the matter and antimatter in the universe annihilated each oth
  307. 14-10 The universe changed from being controlled by radiation to being controlled by matter
  308. THE STRUCTURE OF THE UNIVERSE
  309. 14-11 Galaxies formed from huge clouds of primordial gas
  310. 14-12 Star formation activity determines a galaxy’s initial structure
  311. THE FATE OF THE UNIVERSE
  312. 14-13 The average density of matter is one factor that determines the future of the universe
  313. 14-14 The overall shape of spacetime affects the future of the universe
  314. 14-15 Dark energy is causing the universe to accelerate outward
  315. Summary of Key Ideas
  316. DISCOVERY 14-1 Superstring Theory and M-Theory
  317. CHAPTER 15 Astrobiology
  318. 15-1 Astrobiology connects the cosmos and the origins of life
  319. 15-2 The existence of life depends on chemical and physical properties of matter
  320. 15-3 Evidence is mounting that life might exist elsewhere in our solar system
  321. 15-4 Searches for advanced civilizations try to detect their radio signals
  322. 15-5 The Drake equation: How many civilizations are likely to exist in the Milky Way?
  323. 15-6 Humans have been sending signals into space for more than a century
  324. Summary of Key Ideas
  325. Appendices
  326. A: Powers-of-Ten Notation
  327. B: Temperature Scales
  328. C The Planets: Orbital Data
  329. D: The Planets: Physical Data
  330. E: Major Satellites of the Planets by Mass
  331. F: The Nearest Stars
  332. G: The Visually Brightest Stars
  333. H: The Constellations
  334. I: Some Useful Astronomical Quantities
  335. J: Some Useful Physical Constants
  336. K: Common Conversions between U.S. Customary and Metric Units
  337. L: Mass and Energy Inventory for the Universe
  338. M: Reading Graphs
  339. N: Periodic Table of the Elements
  340. O: Tides
  341. P: Energy and Momentum
  342. Q: Radioactivity and the Ages of Objects
  343. R: Gravitational Force
  344. S: Largest Optical Telescopes in the World
  345. Glossary
  346. A
  347. B
  348. C
  349. D
  350. E
  351. F
  352. G
  353. H
  354. I
  355. J
  356. K
  357. L
  358. M
  359. N
  360. O
  361. P
  362. Q
  363. R
  364. S
  365. T
  366. U
  367. V
  368. W
  369. X
  370. Z
  371. Answers to Computational Questions
  372. Index
  373. A
  374. B
  375. C
  376. D
  377. E
  378. F
  379. G
  380. H
  381. I
  382. J
  383. K
  384. L
  385. M
  386. N
  387. O
  388. P
  389. Q
  390. R
  391. S
  392. T
  393. U
  394. V
  395. W
  396. X
  397. Y
  398. Z
  399. EULA

 

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