Loose Leaf For Explorations: Introduction To Astronomy
9th Edition
ISBN: 9781260432145
Author: Thomas T Arny, Stephen E Schneider Professor
Publisher: McGraw-Hill Education
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Chapter 12, Problem 10P
To determine
The number of years that the Sun should shine.
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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.
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.
1) a) At what rate is the Sun's mass decreasing due to nuclear reactions Am/At? Use E=mc? and
Lsun=3.839x1026 W and give your answer in Msun/year.
b) And due to solar wind? Calculate the flow using v=500 km/s measured on Earth, n=7x106
particles/m³ and µ=1.
c) Assuming that those 2 processes rates remain constant during the Sun's main-sequence
life, would either mass loss process significantly affect the total mass of the Sun? Use that the
Sun's lifetime in the main-sequence is ~ 1010 years.
Chapter 12 Solutions
Loose Leaf For Explorations: Introduction To Astronomy
Ch. 12 - Prob. 1QFRCh. 12 - Prob. 2QFRCh. 12 - Prob. 3QFRCh. 12 - Prob. 4QFRCh. 12 - Prob. 5QFRCh. 12 - Prob. 6QFRCh. 12 - Prob. 7QFRCh. 12 - Prob. 8QFRCh. 12 - Prob. 9QFRCh. 12 - Prob. 10QFR
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- The sun has a radius of 6.959 × 108 m and a surface temperature of 5.81 x 10° K. When the sun radiates at a rate of 3.91 x 1026 W and is a perfect emitter. What is the rate of energy emitted per square meter? Stefan-Boltzmann constant is 5.67 x 10-8 J/s-m2 K4 a) 5.6 x 107 W/m2 b) 12.8 x 107 W/m2 c) 6.4 x 107 W/m2 25.6 x 107 W/m2 5.6 x 1017 W/m2arrow_forwarda.Calculate the mass loss rate of the Sun M˙ due to the solar wind flow. Assume averageproperties of the solar wind of number density 6 protons cm−3, and a flow speed of 450 kms−1. Express your answer in units of both kg per year, and solar masses per year. b.Suppose the solar wind flow is perfectly radial. Calculate the expected rate of change ofsolar rotation frequency dω/dt at the present time, based on conservation of angular momentum. Give your answer in units of rad s−1 y−1(i.e., radians per second per year) and alsoin terms of fractional change per year, i.e., 1/ωdω/dt .Use a current solar rotation period of P = 25.38 days to calculate the current angularfrequency of rotation ω. The moment of inertia of a uniform sphere is 2/5 MR2. You canassume that the radius of the Sun is approximately constant, and the change in its momentof inertia due to the solar wind is only due to the mass loss. c.By observing the rotation period of stars similar to the Sun, it is inferred that their…arrow_forwardConsider the two nuclear reactions I: A + B → C + E II: C + D → F + G(a) Show that the net disintegration energy for these two reactions (Qnet = QI + QII) is identical to the disintegration energy for the net reaction A + B + D → E + F + G(b) One chain of reactions in the Sun’s core is the protonproton cycle. Based on part (a), what is Qnet for this sequence?arrow_forward
- d) Calculate what temperature a thermal kinetic energy of 2 keV corresponds to, and compare this with the temperature in the core of the Sun.arrow_forwardNow suppose that all of the hydrogen atoms in the Sun were converted into helium. How much total energy would be produced? (To calculate the answer, you will have to estimate how many hydrogen atoms are in the Sun. This will give you good practice with scientific notation, since the numbers involved are very large! See Appendix C for a review of scientific notation.)arrow_forwardWhy is fission not an important energy source in the Sun?arrow_forward
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