Astronomy
1st Edition
ISBN: 9781938168284
Author: Andrew Fraknoi; David Morrison; Sidney C. Wolff
Publisher: OpenStax
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Textbook Question
Chapter 22, Problem 5E
Describe the evolution of a star with a mass similar to that of the Sun, from just after it first becomes a red giant to the time it exhausts the last type of fuel its core is capable of fusing.
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Students have asked these similar questions
A red giant star might have radius = 104 times the solar radius,
and luminosity = 1730 times solar luminosity.
Use the data given below to calculate the temperature
at the surface of the red giant star.
Data:
solar radius R = 7 x 108 meters
solar luminosity L = 4 x 1026 watts
Stefan-Boltzmann constant
a = 5.67 x 10-8 W m² K-4
(in K)
A: 1226 OB: 1434 OC: 1678 OD: 1963 OE: 2297 OF: 2688 OG: 3145 OH: 3679
One way to calculate the radius of a star is to use its luminosity and temperature and assume that the star radiates approximately like a blackbody. Astronomers have measured the characteristics of central stars of planetary nebulae and have found that a typical central star is 16 times as luminous and 20 times as hot (about 110,000 K) as the Sun. Find the radius in terms of the Sun’s. How does this radius compare with that of a typical white dwarf?
Betelgeuse is a nearby supergiant that will eventually explode into a supernova. Let's see
how awesome it would look. At peak brightness, the supernova will have a luminosity of
about 10 billion times the Sun. It is 600 light-years away. All stellar brightnesses are
compared with Vega, which has an intrinsic luminosity of about 60 times the Sun, a distance
of 25 light-years, an absolute magnitude of 0.6 and an apparent magnitude of 0 (by
definition).
a) At peak brightness, how many times brighter will Betelgeuse be than Vega?
b) Approximately what apparent magnitude does this correspond to?
c) The Sun is about -26.5 apparent magnitude. What fraction of the Sun's brightness will
Betelgeuse be?
Chapter 22 Solutions
Astronomy
Ch. 22 - Compare the following stages in the lives of a...Ch. 22 - What is the first event that happens to a star...Ch. 22 - Astronomers find that 90% of the stars observed in...Ch. 22 - Describe the evolution of a star with a mass...Ch. 22 - Describe the evolution of a star with a mass...Ch. 22 - A star is often described as “moving” on an HR...Ch. 22 - On which edge of the main sequence band on an HR...Ch. 22 - How do stars typically “move” through the main...Ch. 22 - Certain stars, like Betelgeuse, have a lower...Ch. 22 - Gravity always tries to collapse the mass of a...
Ch. 22 - Why are star clusters so useful for astronomers...Ch. 22 - Would the Sun more likely have been a member of a...Ch. 22 - Suppose you were handed two HR diagrams for two...Ch. 22 - Referring to the HR diagrams in Exercise 22.13,...Ch. 22 - The nuclear process for fusing helium into carbon...Ch. 22 - Pictures of various planetary nebulae show a...Ch. 22 - Describe the two “recycling” mechanisms that are...Ch. 22 - In which of these star groups would you mostly...Ch. 22 - Explain how an HR diagram of the stars in a...Ch. 22 - Where did the carbon atoms in the trunk of a tree...Ch. 22 - What is a planetary nebula? Will we have one...Ch. 22 - Is the Sun on the zero-age main sequence? Explain...Ch. 22 - How are planetary nebulae comparable to a...Ch. 22 - Which of the planets in our solar system have...Ch. 22 - Would you expect to find an earthlike planet (with...Ch. 22 - In the HR diagrams for some young clusters, stars...Ch. 22 - If the Sun were a member of the cluster NGC 2264,...Ch. 22 - If all the stars in a cluster have nearly the same...Ch. 22 - Suppose a star cluster were at such a large...Ch. 22 - Suppose an astronomer known for joking around told...Ch. 22 - Stars that have masses approximately 0.8 times the...Ch. 22 - Automobiles are often used as an analogy to help...Ch. 22 - The text says a star does not change its mass very...Ch. 22 - The text explains that massive stars have shorter...Ch. 22 - You can use the equation in Exercise 22.34 to...Ch. 22 - You can estimate the age of the planetary nebula...Ch. 22 - If star A has a core temperature T, and star B has...
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- What physical properties are different for an M giant with a luminosity of 1000 LSunand an M dwarf with a luminosity of 0.5 LSun? What physical properties are the same?arrow_forwardfill in missing word a) One difference between a type I and type II supernova is the formation of the element _________ in the core that produces a type II supernova b) The Chandrasekhar limit of a star (1.4 solar masses) is the mass limit above which a star cannot remain stable as a ________ ________. c) The temperature of a red giant star is ____________ than it was when the star was a dwarf.arrow_forwardThe mass-luminosity relation describes the mathematical relationship between luminosity and mass for main sequence stars. It describes how a star with a mass of 4 M⊙ would have a luminosity of ______ L⊙. If a star has a radius 1/2 that of the Sun and a temperature 4 that of the Sun, how many times higher is the star's luminosity than that of the Sun? (If it is smaller by a factor of 8, you would write 0.125 because 1/8=0.125) If a star has a radius 2 times larger than the Sun's and a luminosity 1/4th that of the Sun, how many times higher is the star's temperature than that of the Sun? (If it is smaller by a factor of 8, you would write 0.125 because 1/8=0.125) If a star has a surface temperature 2 times lower than the Sun's and a luminosity the same as the Sun, how many times larger is the star than the Sun? (If it is smaller by a factor of 8, you would write 0.125 because 1/8=0.125)arrow_forward
- 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…arrow_forwardThis star has a mass of 3.3 MSun. What is the main sequence lifetime of this star? You may assume that the lifetime of the sun is 1010 yr.arrow_forwardUsing solar units, we find that a star has 4 times the luminosity of the Sun, a mass 1.25 times the mass of the Sun, and a surface temperature of 4090 K (take the Sun's surface temperature to be 5784 K for the sake of this problem). This means the star has a radius of.................... solar radii and is a .................... star (use the classification).arrow_forward
- For a main sequence star with luminosity L, how many kilograms of hydrogen is being converted into helium per second? Use the formula that you derive to estimate the mass of hydrogen atoms that are converted into helium in the interior of the sun (LSun = 3.9 x 1026 W). (Note: the mass of a hydrogen atom is 1 mproton and the mass of a helium atom is 3.97 mproton. You need four hydrogen nuclei to form one helium nucleus.)arrow_forwardA red giant that was originally a 9.5MSun main-sequence star loses a solar mass in 100,000 years via a superwind. What is this mass loss rate in units of solar masses per year? (the answer is not 0.000095 solar masses per year). Additionally, at this mass loss rate, what will the red giant's mass be after 0.5 million years? (Enter your answer as a multiple of MSun.)arrow_forwardPut in order, from earliest to latest, the sequence of events that lead to a star becoming a red giant. If statement A id first, B is second, etc. then enter ABCDEF A) The increase in total energy production causes the envelope to expand and cool. B) Regions around the core that were previously too cool for fusion to occur now begin fusion. C) Hydrogen in the core is completely used up and fusion stops. D) A bigger, cooler and more luminous star has become a red giant. E) Hydrogen fusion in the shell intensifies due to higher temperatures. F) The core, without a source of energy, contracts and heats up.arrow_forward
- A star begins its life with a mass of 5 MSunbut ends its life as a white dwarf with a mass of 0.8 MSun. List the stages in the star’s life during which it most likely lost some of the mass it started with. How did mass loss occur in each stage?arrow_forwardDescribe the evolution of a star with a mass like that of the Sun, from the main-sequence phase of its evolution until it becomes a white dwarf.arrow_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_forward
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