Location via proxy:   [ UP ]  
[Report a bug]   [Manage cookies]                
SlideShare a Scribd company logo

Chapter 12 Test

•
•
D
dlsupport

Stars like our Sun will end their lives as red giants and later contract into white dwarfs. Massive stars create heavy elements through nucleosynthesis. The Sun will evolve away from the main sequence when its hydrogen fuel is exhausted in the core. Stars spend most of their lives on the main sequence fusing hydrogen into helium.

1 of 35
© 2007 Pearson Prentice Hall This work is protected by United States copyright laws and is provided solely for the use of instructors in teaching their courses and assessing student learning. Dissemination or sale of any part of this work (including on the World Wide Web) will destroy the integrity of the work and is not permitted. The work and materials from it should never be made available to students except by instructors using the accompanying text in their classes. All recipients of this work are expected to abide by these restrictions and to honor the intended pedagogical purposes and the needs of other instructors who rely on these materials. Conceptual Test PRS-Enabled Chapter 12 ASTRONOMY, A Beginner’s Guide to the Universe 5 th edition Chaisson McMillan
1) red giants. 2) pulsars. 3) black holes. 4) white dwarfs. 5) red dwarfs. Question 1 Stars like our Sun will end their lives as
1) red giants. 2) pulsars. 3) black holes. 4) white dwarfs. 5) red dwarfs. Question 1 Stars like our Sun will end their lives as Low-mass stars eventually swell into red giants, and their cores later contract into white dwarfs.
Question 2 The elements heavier than Hydrogen and Helium were created 1) in the Big Bang. 2) by nucleosynthesis in massive stars. 3) in the cores of stars like the Sun. 4) within planetary nebulae. 5) They have always existed.
1) in the Big Bang. 2) by nucleosynthesis in massive stars. 3) in the cores of stars like the Sun. 4) within planetary nebula 5) They have always existed. Question 2 The elements heavier than Hydrogen and Helium were created Massive stars create enormous core temperatures as red supergiants, fusing Helium into Carbon, Oxygen, and even heavier elements.
1) its core begins fusing iron. 2) its supply of hydrogen is used up. 3) the carbon core detonates, and it explodes as a Type I supernova. 4) helium builds up in the core, while the hydrogen-burning shell expands. 5) the core loses all of its neutrinos, so all fusion ceases. Question 3 The Sun will evolve away from the main sequence when
1) its core begins fusing iron. 2) its supply of hydrogen is used up. 3) the carbon core detonates, and it explodes as a Type I supernova. 4) helium builds up in the core, while the hydrogen-burning shell expands. 5) the core loses all of its neutrinos, so all fusion ceases. Question 3 The Sun will evolve away from the main sequence when When the Sun’s core becomes unstable and contracts, additional H fusion generates extra pressure, and the star will swell into a red giant.
1) when T-Tauri bipolar jets shoot out. 2) in the middle of the main sequence stage. 3) in the red giant stage. 4) during the formation of a neutron star. 5) in the planetary nebula stage. Question 4 The “helium flash” occurs
1) when T-Tauri bipolar jets shoot out. 2) in the middle of the main sequence stage. 3) in the red giant stage. 4) during the formation of a neutron star. 5) in the planetary nebula stage. Question 4 The “helium flash” occurs When the collapsing core of a red giant reaches high enough temperatures and densities, helium can fuse into carbon quickly – a “helium flash”.
Question 5 Stars gradually lose mass as they become white dwarfs during the 1) T-Tauri stage. 2) emission nebula stage. 3) supernova stage. 4) nova stage. 5) planetary nebula stage.
Question 5 Stars gradually lose mass as they become white dwarfs during the Low mass stars forming white dwarfs slowly lose their outer atmospheres, and illuminate these gases for a relatively short time. 1) T-Tauri stage. 2) emission nebula stage. 3) supernova stage. 4) nova stage. 5) planetary nebula stage.
1) the number of main sequence stars. 2) the ratio of giants to supergiants. 3) the luminosity of stars at the turn-off point. 4) the number of white dwarfs. 5) Supernova explosions. Question 6 Astronomers determine the age of star clusters by observing
1) the number of main sequence stars. 2) the ratio of giants to supergiants. 3) the luminosity of stars at the turn-off point. 4) the number of white dwarfs. 5) Supernova explosions. Question 6 Astronomers determine the age of star clusters by observing The H-R diagram of a cluster can indicate its approximate age. Turn-off point from the main sequence
1) electron degeneracy. 2) neutron degeneracy. 3) thermal pressure from intense core temperatures. 4) gravitational pressure. 5) helium-carbon fusion. Question 7 The source of pressure that makes a white dwarf stable is
1) electron degeneracy. 2) neutron degeneracy. 3) thermal pressure from intense core temperatures. 4) gravitational pressure. 5) helium-carbon fusion. Question 7 The source of pressure that makes a white dwarf stable is Electrons in the core cannot be squeezed infinitely close, and prevent a low-mass star from collapsing further.
1) an asteroid. 2) a planet the size of Earth. 3) a planet the size of Jupiter. 4) an object the size of the Moon. 5) an object the size of a sugar cube. Question 8 In a white dwarf, the mass of the Sun is packed into the volume of
1) an asteroid. 2) a planet the size of Earth. 3) a planet the size of Jupiter. 4) an object the size of the Moon. 5) an object the size of a sugar cube. Question 8 In a white dwarf, the mass of the Sun is packed into the volume of The density of a white dwarf is about a million times greater than normal solid matter.
1) ending their main-sequence stage. 2) also evolving into red giants. 3) forming planetary nebulae. 4) barely starting to fuse Hydrogen. 5) starting the Nova stage. Question 9 In a young star cluster, when more massive stars are evolving into red giants, the least massive stars are
1) ending their main-sequence stage. 2) also evolving into red giants. 3) forming planetary nebulae. 4) barely starting to fuse Hydrogen. 5) starting the Nova stage. Question 9 In a young star cluster, when more massive stars are evolving into red giants, the least massive stars are More massive stars form much faster, and have much shorter main-sequence lifetimes. Low mass stars form more slowly.
1) as a protostar. 2) as a red giant. 3) as a main-sequence star. 4) as a white dwarf. 5) evolving from type O to type M. Question 10 A star will spend most of its “shining” lifetime
1) as a protostar. 2) as a red giant. 3) as a main-sequence star. 4) as a white dwarf. 5) evolving from type O to type M. Question 10 A star will spend most of its “shining” lifetime In the main-sequence stage, hydrogen fuses to helium. Pressure from light and heat pushing out balances gravitational pressure pushing inward.
1) mass transfer onto a white dwarf in a binary star system. 2) repeated helium fusion flashes in red giants. 3) rapid collapse of a protostar into a massive O star. 4) the explosion of a low-mass star. 5) the birth of a massive star in a new cluster. Question 11 A nova involves
1) mass transfer onto a white dwarf in a binary star system. 2) repeated helium fusion flashes in red giants. 3) rapid collapse of a protostar into a massive O star. 4) the explosion of a low-mass star. 5) the birth of a massive star in a new cluster. Question 11 A nova involves Sudden, rapid fusion of new fuel dumped onto a white dwarf causes the star to flare up, and for a short time become much brighter.
1) those heavier than iron, because of supernovae 2) iron, formed just before massive stars explode 3) odd-numbered nuclei, built with hydrogen fusion 4) even-numbered nuclei, built with helium fusion Question 12 What type of atomic nuclei heavier than helium are most common, and why?
1) those heavier than iron, because of supernovae 2) iron, formed just before massive stars explode 3) odd-numbered nuclei, built with hydrogen fusion 4) even-numbered nuclei, built with helium fusion Question 12 What type of atomic nuclei heavier than helium are most common, and why? Helium nuclei have an atomic mass of 4; they act as building blocks in high-temperature fusion within supergiants.
1) its mass exceeds the Chandrasekhar limit. 2) its electron degeneracy increases enormously. 3) fusion reactions increase in their core. 4) Iron in its core collapses. 5) the planetary nebula stage ends. Question 13 A white dwarf can explode when
1) its mass exceeds the Chandrasekhar limit. 2) its electron degeneracy increases enormously. 3) fusion reactions increase in their core. 4) Iron in its core collapses. 5) the planetary nebula stage ends. Question 13 A white dwarf can explode when If additional mass from a companion star pushes a white dwarf beyond 1.4 solar masses, it can explode in a type I supernova.
1) Hydrogen fusion shuts off. 2) Uranium decays into Lead. 3) Iron in the core starts to fuse. 4) Helium is exhausted in the outer layers. 5) a white dwarf gains mass. Question 14 A Type II supernova occurs when
Question 14 A Type II supernova occurs when Fusion of iron does not produce energy or provide pressure; the star’s core collapses immediately triggering a supernova explosion. 1) Hydrogen fusion shuts off. 2) Uranium decays into Lead. 3) Iron in the core starts to fuse. 4) Helium is exhausted in the outer layers. 5) a white dwarf gains mass.
1) its parent star had been studied before the explosion. 2) its distance was already known. 3) it was observed early, as its light was still increasing. 4) its evolution was captured with detailed images from the Hubble Space Telescope. 5) All of the above are true. Question 15 Supernova 1987A was important because
1) its parent star had been studied before the explosion. 2) its distance was already known. 3) it was observed early, as its light was still increasing. 4) its evolution was captured with detailed images from the Hubble Space Telescope. 5) All of the above are true. Question 15 Supernova 1987A was important because Supernovae are important distance indicators in the study of galaxies beyond the Milky Way.
1) they gradually become cooler and dimmer (spectral type O to type M). 2) they gradually become hotter and brighter (spectral type M to type O). 3) they don’t change their spectral type. Question 16 As stars evolve during their main-sequence lifetime
1) they gradually become cooler and dimmer (spectral type O to type M). 2) they gradually become hotter and brighter (spectral type M to type O). 3) they don’t change their spectral type. Question 16 As stars evolve during their main-sequence lifetime A star’s main sequence characteristics of surface temperature and brightness are based on its mass. Stars of different initial mass become different spectral types on the main sequence.
1) hotter 2) smaller 3) larger 4) cooler 5) identical in size Question 17 More massive white dwarfs are ______ compared with less massive white dwarfs.
1) hotter 2) smaller 3) larger 4) cooler 5) identical in size Question 17 More massive white dwarfs are ______ compared with less massive white dwarfs. Chandrasekhar showed that more mass will squeeze a white dwarf into a smaller volume, due to electron degeneracy pressure.

More Related Content

Chapter 12 Test

  • 1. © 2007 Pearson Prentice Hall This work is protected by United States copyright laws and is provided solely for the use of instructors in teaching their courses and assessing student learning. Dissemination or sale of any part of this work (including on the World Wide Web) will destroy the integrity of the work and is not permitted. The work and materials from it should never be made available to students except by instructors using the accompanying text in their classes. All recipients of this work are expected to abide by these restrictions and to honor the intended pedagogical purposes and the needs of other instructors who rely on these materials. Conceptual Test PRS-Enabled Chapter 12 ASTRONOMY, A Beginner’s Guide to the Universe 5 th edition Chaisson McMillan
  • 2. 1) red giants. 2) pulsars. 3) black holes. 4) white dwarfs. 5) red dwarfs. Question 1 Stars like our Sun will end their lives as
  • 3. 1) red giants. 2) pulsars. 3) black holes. 4) white dwarfs. 5) red dwarfs. Question 1 Stars like our Sun will end their lives as Low-mass stars eventually swell into red giants, and their cores later contract into white dwarfs.
  • 4. Question 2 The elements heavier than Hydrogen and Helium were created 1) in the Big Bang. 2) by nucleosynthesis in massive stars. 3) in the cores of stars like the Sun. 4) within planetary nebulae. 5) They have always existed.
  • 5. 1) in the Big Bang. 2) by nucleosynthesis in massive stars. 3) in the cores of stars like the Sun. 4) within planetary nebula 5) They have always existed. Question 2 The elements heavier than Hydrogen and Helium were created Massive stars create enormous core temperatures as red supergiants, fusing Helium into Carbon, Oxygen, and even heavier elements.
  • 6. 1) its core begins fusing iron. 2) its supply of hydrogen is used up. 3) the carbon core detonates, and it explodes as a Type I supernova. 4) helium builds up in the core, while the hydrogen-burning shell expands. 5) the core loses all of its neutrinos, so all fusion ceases. Question 3 The Sun will evolve away from the main sequence when
  • 7. 1) its core begins fusing iron. 2) its supply of hydrogen is used up. 3) the carbon core detonates, and it explodes as a Type I supernova. 4) helium builds up in the core, while the hydrogen-burning shell expands. 5) the core loses all of its neutrinos, so all fusion ceases. Question 3 The Sun will evolve away from the main sequence when When the Sun’s core becomes unstable and contracts, additional H fusion generates extra pressure, and the star will swell into a red giant.
  • 8. 1) when T-Tauri bipolar jets shoot out. 2) in the middle of the main sequence stage. 3) in the red giant stage. 4) during the formation of a neutron star. 5) in the planetary nebula stage. Question 4 The “helium flash” occurs
  • 9. 1) when T-Tauri bipolar jets shoot out. 2) in the middle of the main sequence stage. 3) in the red giant stage. 4) during the formation of a neutron star. 5) in the planetary nebula stage. Question 4 The “helium flash” occurs When the collapsing core of a red giant reaches high enough temperatures and densities, helium can fuse into carbon quickly – a “helium flash”.
  • 10. Question 5 Stars gradually lose mass as they become white dwarfs during the 1) T-Tauri stage. 2) emission nebula stage. 3) supernova stage. 4) nova stage. 5) planetary nebula stage.
  • 11. Question 5 Stars gradually lose mass as they become white dwarfs during the Low mass stars forming white dwarfs slowly lose their outer atmospheres, and illuminate these gases for a relatively short time. 1) T-Tauri stage. 2) emission nebula stage. 3) supernova stage. 4) nova stage. 5) planetary nebula stage.
  • 12. 1) the number of main sequence stars. 2) the ratio of giants to supergiants. 3) the luminosity of stars at the turn-off point. 4) the number of white dwarfs. 5) Supernova explosions. Question 6 Astronomers determine the age of star clusters by observing
  • 13. 1) the number of main sequence stars. 2) the ratio of giants to supergiants. 3) the luminosity of stars at the turn-off point. 4) the number of white dwarfs. 5) Supernova explosions. Question 6 Astronomers determine the age of star clusters by observing The H-R diagram of a cluster can indicate its approximate age. Turn-off point from the main sequence
  • 14. 1) electron degeneracy. 2) neutron degeneracy. 3) thermal pressure from intense core temperatures. 4) gravitational pressure. 5) helium-carbon fusion. Question 7 The source of pressure that makes a white dwarf stable is
  • 15. 1) electron degeneracy. 2) neutron degeneracy. 3) thermal pressure from intense core temperatures. 4) gravitational pressure. 5) helium-carbon fusion. Question 7 The source of pressure that makes a white dwarf stable is Electrons in the core cannot be squeezed infinitely close, and prevent a low-mass star from collapsing further.
  • 16. 1) an asteroid. 2) a planet the size of Earth. 3) a planet the size of Jupiter. 4) an object the size of the Moon. 5) an object the size of a sugar cube. Question 8 In a white dwarf, the mass of the Sun is packed into the volume of
  • 17. 1) an asteroid. 2) a planet the size of Earth. 3) a planet the size of Jupiter. 4) an object the size of the Moon. 5) an object the size of a sugar cube. Question 8 In a white dwarf, the mass of the Sun is packed into the volume of The density of a white dwarf is about a million times greater than normal solid matter.
  • 18. 1) ending their main-sequence stage. 2) also evolving into red giants. 3) forming planetary nebulae. 4) barely starting to fuse Hydrogen. 5) starting the Nova stage. Question 9 In a young star cluster, when more massive stars are evolving into red giants, the least massive stars are
  • 19. 1) ending their main-sequence stage. 2) also evolving into red giants. 3) forming planetary nebulae. 4) barely starting to fuse Hydrogen. 5) starting the Nova stage. Question 9 In a young star cluster, when more massive stars are evolving into red giants, the least massive stars are More massive stars form much faster, and have much shorter main-sequence lifetimes. Low mass stars form more slowly.
  • 20. 1) as a protostar. 2) as a red giant. 3) as a main-sequence star. 4) as a white dwarf. 5) evolving from type O to type M. Question 10 A star will spend most of its “shining” lifetime
  • 21. 1) as a protostar. 2) as a red giant. 3) as a main-sequence star. 4) as a white dwarf. 5) evolving from type O to type M. Question 10 A star will spend most of its “shining” lifetime In the main-sequence stage, hydrogen fuses to helium. Pressure from light and heat pushing out balances gravitational pressure pushing inward.
  • 22. 1) mass transfer onto a white dwarf in a binary star system. 2) repeated helium fusion flashes in red giants. 3) rapid collapse of a protostar into a massive O star. 4) the explosion of a low-mass star. 5) the birth of a massive star in a new cluster. Question 11 A nova involves
  • 23. 1) mass transfer onto a white dwarf in a binary star system. 2) repeated helium fusion flashes in red giants. 3) rapid collapse of a protostar into a massive O star. 4) the explosion of a low-mass star. 5) the birth of a massive star in a new cluster. Question 11 A nova involves Sudden, rapid fusion of new fuel dumped onto a white dwarf causes the star to flare up, and for a short time become much brighter.
  • 24. 1) those heavier than iron, because of supernovae 2) iron, formed just before massive stars explode 3) odd-numbered nuclei, built with hydrogen fusion 4) even-numbered nuclei, built with helium fusion Question 12 What type of atomic nuclei heavier than helium are most common, and why?
  • 25. 1) those heavier than iron, because of supernovae 2) iron, formed just before massive stars explode 3) odd-numbered nuclei, built with hydrogen fusion 4) even-numbered nuclei, built with helium fusion Question 12 What type of atomic nuclei heavier than helium are most common, and why? Helium nuclei have an atomic mass of 4; they act as building blocks in high-temperature fusion within supergiants.
  • 26. 1) its mass exceeds the Chandrasekhar limit. 2) its electron degeneracy increases enormously. 3) fusion reactions increase in their core. 4) Iron in its core collapses. 5) the planetary nebula stage ends. Question 13 A white dwarf can explode when
  • 27. 1) its mass exceeds the Chandrasekhar limit. 2) its electron degeneracy increases enormously. 3) fusion reactions increase in their core. 4) Iron in its core collapses. 5) the planetary nebula stage ends. Question 13 A white dwarf can explode when If additional mass from a companion star pushes a white dwarf beyond 1.4 solar masses, it can explode in a type I supernova.
  • 28. 1) Hydrogen fusion shuts off. 2) Uranium decays into Lead. 3) Iron in the core starts to fuse. 4) Helium is exhausted in the outer layers. 5) a white dwarf gains mass. Question 14 A Type II supernova occurs when
  • 29. Question 14 A Type II supernova occurs when Fusion of iron does not produce energy or provide pressure; the star’s core collapses immediately triggering a supernova explosion. 1) Hydrogen fusion shuts off. 2) Uranium decays into Lead. 3) Iron in the core starts to fuse. 4) Helium is exhausted in the outer layers. 5) a white dwarf gains mass.
  • 30. 1) its parent star had been studied before the explosion. 2) its distance was already known. 3) it was observed early, as its light was still increasing. 4) its evolution was captured with detailed images from the Hubble Space Telescope. 5) All of the above are true. Question 15 Supernova 1987A was important because
  • 31. 1) its parent star had been studied before the explosion. 2) its distance was already known. 3) it was observed early, as its light was still increasing. 4) its evolution was captured with detailed images from the Hubble Space Telescope. 5) All of the above are true. Question 15 Supernova 1987A was important because Supernovae are important distance indicators in the study of galaxies beyond the Milky Way.
  • 32. 1) they gradually become cooler and dimmer (spectral type O to type M). 2) they gradually become hotter and brighter (spectral type M to type O). 3) they don’t change their spectral type. Question 16 As stars evolve during their main-sequence lifetime
  • 33. 1) they gradually become cooler and dimmer (spectral type O to type M). 2) they gradually become hotter and brighter (spectral type M to type O). 3) they don’t change their spectral type. Question 16 As stars evolve during their main-sequence lifetime A star’s main sequence characteristics of surface temperature and brightness are based on its mass. Stars of different initial mass become different spectral types on the main sequence.
  • 34. 1) hotter 2) smaller 3) larger 4) cooler 5) identical in size Question 17 More massive white dwarfs are ______ compared with less massive white dwarfs.
  • 35. 1) hotter 2) smaller 3) larger 4) cooler 5) identical in size Question 17 More massive white dwarfs are ______ compared with less massive white dwarfs. Chandrasekhar showed that more mass will squeeze a white dwarf into a smaller volume, due to electron degeneracy pressure.