Universe Tenth Edition Roger Freedman • Robert Geller • William Kaufmann III Universe Tenth Edition Clicker Questions Chapter 16 Our Star, the Sun

Stars in different stages of their evolution may generate energy using different nuclear reactions. These reactions can occur in the core or in a layer around the core. At the present, the energy of the Sun is generated in its central core by fission of heavy nuclei. from gravitational energy as the Sun slowly shrinks. in its core by radioactive decay of uranium. in the central core by fusion of helium nuclei and in an outer shell by fusion of hydrogen nuclei. in its central core by fusion of hydrogen nuclei. Q16.1

Stars in different stages of their evolution may generate energy using different nuclear reactions. These reactions can occur in the core or in a layer around the core. At the present, the energy of the Sun is generated in its central core by fission of heavy nuclei. from gravitational energy as the Sun slowly shrinks. in its core by radioactive decay of uranium. in the central core by fusion of helium nuclei and in an outer shell by fusion of hydrogen nuclei. in its central core by fusion of hydrogen nuclei. A16.1

The “fuel” of the Sun is ______, and the main products of the nuclear reactions include ______. hydrogen / helium, neutrinos, and gamma rays helium / only neutrinos and gamma rays hydrogen / neutrinos and microwaves helium / neutrinos and microwaves hydrogen / only neutrinos. Q16.2

The “fuel” of the Sun is ______, and the main products of the nuclear reactions include ______. hydrogen / helium, neutrinos, and gamma rays helium / only neutrinos and gamma rays hydrogen / neutrinos and microwaves helium / neutrinos and microwaves hydrogen / only neutrinos. A16.2

Which of the following best describes a positron? Another name for a proton A particle with no charge and little or no mass A very short wavelength photon A positively charged electron A negatively charged proton Q16.3

Which of the following best describes a positron? Another name for a proton A particle with no charge and little or no mass A very short wavelength photon A positively charged electron A negatively charged proton A16.3

How do the electron and the neutrino differ? There is no difference between them. The neutrino has no charge, a much smaller mass than the electron, and interacts weakly with matter. The neutrino has no charge, a mass the same as the electron, and interacts weakly with matter. The neutrino has the same charge and mass as an electron, and interacts weakly with matter. The neutrino has no charge, a much smaller mass than the electron, and interacts strongly with matter. Q16.4

How do the electron and the neutrino differ? There is no difference between them. The neutrino has no charge, a much smaller mass than the electron, and interacts weakly with matter. The neutrino has no charge, a mass the same as the electron, and interacts weakly with matter. The neutrino has the same charge and mass as an electron, and interacts weakly with matter. The neutrino has no charge, a much smaller mass than the electron, and interacts strongly with matter. A16.4

The energy produced in the central core of the Sun is transported to the surface by radiation in the layers just outside the central core and by convection in the outer layers. by convection in the layers just outside the central core and by radiation in the outer layers. by convection from just outside the central core all the way to the surface. by radiation from just outside the central core all the way to the surface. only by convection. Q16.5

The energy produced in the central core of the Sun is transported to the surface by radiation in the layers just outside the central core and by convection in the outer layers. by convection in the layers just outside the central core and by radiation in the outer layers. by convection from just outside the central core all the way to the surface. by radiation from just outside the central core all the way to the surface. only by convection. A16.5

One of the processes carrying energy from the core of the Sun to its surface is convection. The process of convection involves the motion of hot gases. the conduction of energy from atom to atom. the passing of radiation through the layers of the Sun. the fusion of hydrogen into helium. the decay of radioactive elements. Q16.6

One of the processes carrying energy from the core of the Sun to its surface is convection. The process of convection involves the motion of hot gases. the conduction of energy from atom to atom. the passing of radiation through the layers of the Sun. the fusion of hydrogen into helium. the decay of radioactive elements. A16.6

The surface layers of the Sun are very massive The surface layers of the Sun are very massive. What stops the Sun from collapsing under its own weight? The strong nuclear repulsion between the atoms of these layers. Neutrinos exert a strong outward pressure, holding the layers up. The magnetic field exerts a strong force. The pressure of the very high-temperature gas within the Sun supports the outer layers. The interior of the Sun is under such high pressure that it is solid. Q16.7

The surface layers of the Sun are very massive The surface layers of the Sun are very massive. What stops the Sun from collapsing under its own weight? The strong nuclear repulsion between the atoms of these layers. Neutrinos exert a strong outward pressure, holding the layers up. The magnetic field exerts a strong force. The pressure of the very high-temperature gas within the Sun supports the outer layers. The interior of the Sun is under such high pressure that it is solid. A16.7

The visible spectrum of the Sun contains dark absorption and bright emission lines on a continuous background. is a bright continuous spectrum, containing numerous absorption lines created by the atmosphere of the Sun. consists of only a few bright emission lines. consists of only a few bright absorption lines. is a bright continuous spectrum with no absorption lines. Q16.8

The visible spectrum of the Sun contains dark absorption and bright emission lines on a continuous background. is a bright continuous spectrum, containing numerous absorption lines created by the atmosphere of the Sun. consists of only a few bright emission lines. consists of only a few bright absorption lines. is a bright continuous spectrum with no absorption lines. A16.8

This photo shows solar granulation This photo shows solar granulation. The darker areas are regions where the gas is hotter. cooler. Doppler shifted. moving laterally. less dense. Q16.9

This photo shows solar granulation This photo shows solar granulation. The darker areas are regions where the gas is hotter. cooler. Doppler shifted. moving laterally. less dense. A16.9

Solar flares are explosive eruptions on the Sun’s surface associated with sudden movements of the Sun’s magnetic field. At what places on the surface of the Sun do solar flares usually originate? Within an isolated pair of sunspots Within a complex group of sunspots At the north and south poles of the Sun Anywhere on the equator of the Sun In the solar corona Q16.10

Solar flares are explosive eruptions on the Sun’s surface associated with sudden movements of the Sun’s magnetic field. At what places on the surface of the Sun do solar flares usually originate? Within an isolated pair of sunspots Within a complex group of sunspots At the north and south poles of the Sun Anywhere on the equator of the Sun In the solar corona A16.10

The dark regions on this photo of the Sun are the corona. solar granules. Zeeman effects. sunspots. prominences. Q16.11

The dark regions on this photo of the Sun are the corona. solar granules. Zeeman effects. sunspots. prominences. A16.11

How does the temperature in the umbra of a sunspot compare to that of the photosphere outside the sunspot? The umbra is about 1500 K cooler. The umbra is about 1500 K hotter. The umbra is about 4300 K hotter. The umbra is about 4300 K cooler. The umbra and photosphere are at about the same temperature. Q16.12

How does the temperature in the umbra of a sunspot compare to that of the photosphere outside the sunspot? The umbra is about 1500 K cooler. The umbra is about 1500 K hotter. The umbra is about 4300 K hotter. The umbra is about 4300 K cooler. The umbra and photosphere are at about the same temperature. A16.12

The bright white regions in this photo of the Sun are an upheaval of material injected into the Sun’s photosphere. magnetic field. corona. chromosphere. interior. Q16.13

The bright white regions in this photo of the Sun are an upheaval of material injected into the Sun’s photosphere. magnetic field. corona. chromosphere. interior. A16.13