21ST C ASTRO EBOOK+SW5=SS+VGCRD+LEARN/DO
6th Edition
ISBN: 9780393870152
Author: PALEN
Publisher: Norton, W. W. & Company, Inc.
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Chapter 16, Problem 43QP
To determine
The density of degenerate material and radius of sun.
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The average density of the sun is 1. 4 g/cm3 What do you expect the density to be at 0.25 of Rsun?
2)
The average density of the sun is 1.4 g/cm3.
The following resource claims that the sun's core has a density of 150 g/cm3 and a radius of 25% of the sun's radius. Assume the core has a constant density and calculate it's mass.
What fraction of the sun's mass is in the core according to that resource?
Describe the reaction that powers the sun during its main sequence lifetime. Be sure to include
the basic ingredients and the basic products.
A Crude Analysis:
In about 5 billion years, the Sun is going to look a lot different. Our
sun is going to turn into a red-giant, a bigger star whose core
temperature is much higher than the Sun's current core temperature
(you will learn about the red giants in the coming weeks). Assume
the core temperature of the red-giant phase of the Sun does not go
beyond 100 million degrees.
Do you think the temperature is high enough for helium fusion to
occur? Note that this question is about helium fusion not hydrogen
fusion. How are you going about proving your claim?
Question: What temperature in degrees Kelvin must the red-giant
sun be at to allow for the helium-helium interactions to take place
not considering the Quantum Mechanical effects (i.e. what
temperature would allow helium atoms to breach the helium-helium
potential wall without help from Quantum Mechanics)? Use wolfram
alpha to find the values for the constants. Round your answer to two
decimal places.
Your answer i [ Select ]
1.47…
Chapter 16 Solutions
21ST C ASTRO EBOOK+SW5=SS+VGCRD+LEARN/DO
Ch. 16.1 - Prob. 16.1CYUCh. 16.3 - Prob. 16.3CYUCh. 16.4 - Prob. 16.4CYUCh. 16.5 - Prob. 16.5CYUCh. 16 - Prob. 1QPCh. 16 - Prob. 2QPCh. 16 - Prob. 3QPCh. 16 - Prob. 4QPCh. 16 - Prob. 5QPCh. 16 - Prob. 6QP
Ch. 16 - Prob. 8QPCh. 16 - Prob. 9QPCh. 16 - Prob. 10QPCh. 16 - Prob. 11QPCh. 16 - Prob. 12QPCh. 16 - Prob. 13QPCh. 16 - Prob. 14QPCh. 16 - Prob. 15QPCh. 16 - Prob. 16QPCh. 16 - Prob. 17QPCh. 16 - Prob. 18QPCh. 16 - Prob. 19QPCh. 16 - Prob. 20QPCh. 16 - Prob. 21QPCh. 16 - Prob. 23QPCh. 16 - Prob. 24QPCh. 16 - Prob. 25QPCh. 16 - Prob. 26QPCh. 16 - Prob. 27QPCh. 16 - Prob. 28QPCh. 16 - Prob. 29QPCh. 16 - Prob. 30QPCh. 16 - Prob. 31QPCh. 16 - Prob. 32QPCh. 16 - Prob. 33QPCh. 16 - Prob. 34QPCh. 16 - Prob. 35QPCh. 16 - Prob. 36QPCh. 16 - Prob. 37QPCh. 16 - Prob. 38QPCh. 16 - Prob. 39QPCh. 16 - Prob. 40QPCh. 16 - Prob. 41QPCh. 16 - Prob. 42QPCh. 16 - Prob. 43QPCh. 16 - Prob. 44QPCh. 16 - Prob. 45QP
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- Which of the below is a possible evolutionary outcome for the Sun (given in the correct chronological order). a) planetary nebula, red giant, white dwarf b) Red giant, planetary nebula, white dwarf c) Red giant, planetary nebula, neutron star d) Red giant, neutron star with simultaneous supernova explosion e) Red giant, black hole with simultaneous supernova explosionarrow_forwardDescribe the evolution of a star with a mass similar to that of the Sun, from the protostar stage to the time it first becomes a red giant. Give the description in words and then sketch the evolution on an HR diagram.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_forward
- A star's Zero Age Main Sequence (ZAMS) radius R, luminosity L, and effective temperature Teff depend primarily on the star's mass. These parameters do evolve somewhat over time, however, while the star still remains on the main sequence. Discuss in what direction each of these parameters evolves, and explain why this occurs. By physical in your explanation. How did this evolution affect our own solar system, if at all?arrow_forwardCan i get help with this three questions about solar masses : 1.What is the significance of 8 solar masses in stellar evolution?2. How does the death of one very massive star give birth to perhaps hundreds of smaller ones soon thereafter?3. Looking at the elements that make up our world, which are the products of low versus high mass stars?arrow_forwardAssume that Hydrogen comprises 79% of the Sun's mass. How much mass is this? 1.57e+30 kg Only 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 inital H in the core of the Sun? Hint: Use the answer above and the percent in the core to determine the total mass. Using the results from above, how much total energy is available to the Sun via nuclear fusion over its lifetime? (HINT: only 0.71% of the total mass of the available H in the core is converted into energy) Hint: E = m c^2arrow_forward
- How would the interior temperature of the Sun be different if the strong force that binds nuclei together were 10 times as strong?arrow_forwarda) At solar maximum sunspots might cover up to 0.4% of the total area of the Sun. If the sunspots have a temperature of 3800 K and the surrounding photosphere has a temperature of 6000 K, calculate the fractional change (as a percentage) in the luminosity due to the presence of the sunspots. b) A star of the same stellar class as the Sun is observed regularly over many years, and a time series of its bolometric apparent magnitude is collected. What would be the signal in this time series which indicated that the star had a magnetic dynamo similar to the Sun? Briefly describe two or three possible sources of other signals which could confuse the interpretation of the data.arrow_forward. The radius of the nebula is about 0.401 light-years. The gas is expanding away from the star at a rate of about 37 kilometers/second . Considering that distance = velocity x time, calculate how long ago the gas left the star if its speed has been constant the whole time. Make sure you use consistent units for time, speed, and distance. Answer in years.arrow_forward
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