UNIVERSE (LOOSELEAF):STARS+GALAXIES
6th Edition
ISBN: 9781319115043
Author: Freedman
Publisher: MAC HIGHER
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Chapter 20, Problem 49Q
To determine
The meaning of core bounce and the way neutrinos contribute to the effects of a core bounce.
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.Explain proton-proton cycle of the energy production in stars using appropriate fusionreactions and schematic figures.
Explain neutrino oscillations and their consequences.
Guide Questions:1. What is the common end-product of proton-proton chain reaction and CNO cycle?2. Why is CNO cycle important in stellar formation and evolution?
Chapter 20 Solutions
UNIVERSE (LOOSELEAF):STARS+GALAXIES
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Need a deep-dive on the concept behind this application? Look no further. Learn more about this topic, physics and related others by exploring similar questions and additional content below.Similar questions
- Do neutrinos have mass? Describe how the answer to this question has changed over time and why.arrow_forwardMultiple Choice During the intermediate step of solar nuclear fusion a. 1 deuterium fuse with 1 proton making helium-3 b. 2 protons fuse together making helium-3 c. 2 deuterium nuclei fuse together making helium-3 d. 1 deuterium fuse with 1 proton making helium-4arrow_forwardCan you respond the questions with a brief description?arrow_forward
- Explain how critical temperature and critical pressure occur. You can also site an example to thoroughly explain.arrow_forwardBased on what you learned about the source of stellar energy and how stars make energy, select all of the correct statements from the following list. 1. Many stars make energy with the proton-proton cycle. 2. The CNO cycle is more efficient than the proton-proton cycle. 3. The sun's energy comes from the CNO cycle.More massive stars make energy with the proton-proton cycle. 4. The leftover mass in both the proton-proton cycle and the CNO cycle is converted to energy. 5. A helium atom is more massive than four hydrogen atoms. 6. The CNO cycle requires a higher temperature than the proton-proton cycle.arrow_forwardDescribe the reaction that powers the sun during its main sequence lifetime. Be sure to include the basic ingredients and the basic products.arrow_forward
- Activity 8: Complete Me! Directions: Complete the given following nuclear reactions on the formation of heavier elements during star formation and evolution. Write your answers in the space given. 1. n° → p* + - + v 2. p* + n° - 12D +- 3. 23He + 12_ 24He + p* 4. 12D + 12D - 24He + 5. 137 + 12D → 24He + - 6. 12H + 12H - 24He + 7. 13H +H 24He + - 8. _- 37Li + 9. + 47B + 10 -- 67C + - Q1 Week 1 (Learning Activity Worksheet) Target Competency: Give evidence for and describe the formation of heavier elements during star formation and evolution. (S11/12PS-lla-2) Page 4 of 8arrow_forwardI need the answer as soon as possiblearrow_forwardStatus of Sun's core and its temperature (The letters correspond to the stages in Figure 21.1.) 3. Stage A: T10 million K. Sun is in equilibrium. 4. Stage B: T 100 million K Core collapse stops. 5. Stage C: Helium flash 6. Stage D: T 100 million K. Sun is in equilibrium. 7. Stage E: T800 million K. Core collapse stops. If fusion is occurring in core or in shell around the core, mark with a ✔in the correct column. Core fusion H to He FUSION ✓ Core fusion He to C Shell fusion H to He Shell fusion He to C PRESSURE VERSUS GRAVITY CORE • REST OF THE STAR Pressure comes from electron degeneracy Pressure Gravity Gravity Pressure region contracts and heats Pressure > Gravity region expands and coolsarrow_forward
- Imagine sensors observe an X4 solar flare and fast-moving 'halo' CME. What sort of response would we expect to see in the 'energetic protons' measured at Earth (i.e. proton event)?Provide a brief description, focusing on the timing and duration of the proton event.arrow_forward1. A planetary nebula has an angular diameter of 76 arc seconds and a distance of 5100 ly. What is its linear diameter (in ly)? Hint: Use the small-angle formula: angular diameter (in arc seconds) 2.06 ✕ 105 = linear diameter distance 2. Suppose a planetary nebula is 3.2 pc in diameter, and Doppler shifts in its spectrum show that the planetary nebula is expanding at 31 km/s. How old is the planetary nebula in yr? (Note: 1 pc = 3.1 ✕ 1013 km and 1 yr = 3.2 ✕ 107 s.)arrow_forwardExplain in detailarrow_forward
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