EXPLORATIONS:INTRO.TO ASTRONOMY
9th Edition
ISBN: 9781260150513
Author: ARNY
Publisher: RENT MCG
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Chapter 12, Problem 10P
To determine
The number of years that the Sun should shine.
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About 2% of the energy generated in the Sun’s core by the p-p reaction is carried out of the Sun by neutrinos. Is the energy associated with this neutrino flux equal to, greater than, or less than the energy radiated from the Sun’s surface as electromagnetic radiation?
Assume that the core of the Sun has one-eighth of the Sun’s mass and is compressed within a sphere whose radius is one-fourth of the solar radius.Assume further that the composition of the core is 31% hydrogen by mass and that essentially all the Sun’s energy is generated there. If the Sun continues to burn hydrogen at the current rate of 6.33E11 kg/s, how long, in years, will it be before the hydrogen is entirely consumed? Mass of the Sun is 2.0x1030 kg.
Assume that the core of the Sun has one-eighth of the Sun’s mass and is compressed within a sphere whose radius is one-fourth of the solar radius.Assume further that the composition of the core is 35% hydrogen by mass and that essentially all the Sun’s energy is generated there. If the Sun continues to burn hydrogen at the current rate of 6.2 *1011 kg/s, how long will it be before the hydrogen is entirely consumed? The Sun’s mass is 2.0 * 1030 kg.
Chapter 12 Solutions
EXPLORATIONS:INTRO.TO ASTRONOMY
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- Why is fission not an important energy source in the Sun?arrow_forwardThe Sun is powered by releasing hydrogen to helium. Through either the proton-proton chain or the CNO cycle, the basic reaction is 4 1H morph into 1 4He, releasing nuclear binding energy (and losing mass) in the process. The mass of one proton 1H is 1.6726 x 10-24 gm and the mass of one helium nucleus 4He is 6.6447 x 10-24 gm. What is the mass difference in gm between 4 protons and one helium nucleus? Calculate the ratio of the mass difference to the original mass of the 4 protons as a comparison.arrow_forwardThe proton – proton cycle responsible for the Sun’s 3.84 x 1026 W power output yields about 26.7 MeV of energy for every four protons that are fused into a helium nucleus. Determine (a) the energy in joules released during each proton – proton cycle fusion reaction, (b) the number of proton – proton cycles occurring per second in the Sun, and (c) the change in the Sun’s mass each second due to this energy release.arrow_forward
- In class I derived the ordinary nuclear density to be about 0.138 u/fm3. A neutron star is a collapsed star that contains neutrons in a highly compactified state, so its average density is higher. Assume a neutron star is spherical and has an average density which is about twice the ordinary nuclear density. If it is 50% heavier than the Sun, what would be its radius? (Given: mass of sun = 2*1030 kg, 1 u = 1.66*10-27 kg.) A) 14.6 km B) 11.6 km C) 10.1 km D) none of these.arrow_forwardThe sun generates its energy through nuclear fusion, making helium from hydrogen. The main process by which this happens, called the proton-proton chain, goes as follows: Two protons come together to create deuterium, a positron, a neutrino, and energy: p + p ⟶ D + e+ + ν + energy The deuterium fuses with another proton to make 3He: D + p ⟶ 3He + energy Fianlly, 4He is produced by fusing two 3He nuclei together: 3He + 3He ⟶ 4He + p + p + energy What is the total energy released during the creation of one 4He nucleus? Give your answer in MeV, and remember that you need to make two 3He nuclei in the process. Be sure to use at least five significant figures for your masses, but your final answer should have three or four sig figs.arrow_forwardSuppose thermonuclear fusion in the Sun’s core stopped abruptly. Would the intensity of sunlight decrease just as abruptly? Why or why not?arrow_forward
- As we’ve seen, the sun’s energy comes from fusion reactions that combine four hydrogen atoms to produce a single helium atom. Even in the sun’s core, where these reactions proceed most rapidly, the reaction rate is very slow, with only about 6.7 * 1013 reactions per second occurring in 1 cubic meter ofthe core. How much power is produced by these fusion reactions per cubic meter? Compare this number with the 300 W/m3 metabolic power produced by a resting reptile.arrow_forwardOnly about 11% of the initial Hydrogen in the Sun is in the core where it is hot enough to burn. What was the total mass of the initial H in the core of the Sun?arrow_forwardOnly about 11% of the initial Hydrogen in the Sun is in the core where it is hot enough to burn. What was the total mass of the initial H in the core of the Sun? (Mass of the Sun is 1.989 × 10^30 kg)arrow_forward
- The Sun and all Main Sequence stars derive their luminosity by fusing hydrogen to helium; in particular 4 1H ® 1 4He + Energy (photons) The mass of a proton is 1.0078 AMU, while the mass of a helium nucleus is 4.0026 AMU. a) How much mass is ``lost'' (in AMU and kg) in fusing four H atoms to one helium? This is called the mass defect. b) Mass isn't really lost, of course. It is converted to energy via E=mc2. How much energy in joules (J) is liberated in a single reaction? c) How many reactions per second are required to account for the entire luminosity of the Sun?arrow_forwardWhy do you suppose so great a fraction of the Sun’s energy comes from its central regions? Within what fraction of the Sun’s radius does practically all of the Sun’s luminosity originate (see Figure 16.16)? Within what radius of the Sun has its original hydrogen been partially used up? Discuss what relationship the answers to these questions bear to one another. Figure 16.16 shows how the temperature, density, rate of energy generation, and composition vary from the center of the Sun to its surface.arrow_forwardSuppose the proton-proton cycle in the Sun were to slow down suddenly and generate energy at only 95% of its current rate. Would an observer on Earth see an immediate decrease in the Sun’s brightness? Would she immediately see a decrease in the number of neutrinos emitted by the Sun?arrow_forward
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