Chapter 22 Stars from Adolescence to Old Age
22.7 Collaborative Group Activities, Questions and Exercises
Collaborative Group Activities
- Have your group take a look at the list of the brightest stars in the sky in Appendix Brightest Stars. What fraction of them are past the main-sequence phase of evolution? The text says that stars spend 90% of their lifetimes in the main-sequence phase of evolution. This suggests that if we have a fair (or representative) sample of stars, 90% of them should be main-sequence stars. Your group should brainstorm why 90% of the brightest stars are not in the main-sequence phase of evolution.
- Reading an H–R diagram can be tricky. Suppose your group is given the H–R diagram of a star cluster. Stars above and to the right of the main sequence could be either red giants that had evolved away from the main sequence or very young stars that are still evolving toward the main sequence. Discuss how you would decide which they are.
- In the chapter on Life in the Universe, we discuss some of the efforts now underway to search for radio signals from possible intelligent civilizations around other stars. Our present resources for carrying out such searches are very limited and there are many stars in our Galaxy. Your group is a committee set up by the International Astronomical Union to come up with a list of the best possible stars with which such a search should begin. Make a list of criteria for choosing the stars on the list, and explain the reasons behind each entry (keeping in mind some of the ideas about the life story of stars and timescales that we discuss in the present chapter.)
- Have your group make a list of the reasons why a star that formed at the very beginning of the universe (soon after the Big Bang) could not have a planet with astronomy students reading astronomy textbooks (even if the star has the same mass as that of our Sun).
- Since we are pretty sure that when the Sun becomes a giant star, all life on Earth will be wiped out, does your group think that we should start making preparations of any kind? Let’s suppose that a political leader who fell asleep during large parts of his astronomy class suddenly hears about this problem from a large donor and appoints your group as a task force to make suggestions on how to prepare for the end of Earth. Make a list of arguments for why such a task force is not really necessary.
- Use star charts to identify at least one open cluster visible at this time of the year. (Such charts can be found in Sky & Telescope and Astronomy magazines each month and their websites;) The Pleiades and Hyades are good autumn subjects, and Praesepe is good for springtime viewing. Go out and look at these clusters with binoculars and describe what you see.
- Many astronomers think that planetary nebulae are among the most attractive and interesting objects we can see in the Galaxy. In this chapter, we could only show you a few examples of the pictures of these objects taken with the Hubble or large telescopes on the ground. Have members of your group search further for planetary nebula images online, and make a “top ten” list of your favourite ones (do not include more than three that were featured in this chapter.) Make a report (with images) for the whole class and explain why you found your top five especially interesting. (You may want to check out the [image of model] from earlier in the chapter in the process.)
Review Questions
1: Compare the following stages in the lives of a human being and a star: prenatal, birth, adolescence/adulthood, middle age, old age, and death. What does a star with the mass of our Sun do in each of these stages?
2: What is the first event that happens to a star with roughly the mass of our Sun that exhausts the hydrogen in its core and stops the generation of energy by the nuclear fusion of hydrogen to helium? Describe the sequence of events that the star undergoes.
3: Astronomers find that 90% of the stars observed in the sky are on the main sequence of an H–R diagram; why does this make sense? Why are there far fewer stars in the giant and supergiant region?
4: Describe 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 H–R diagram.
5: 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.
6: A star is often described as “moving” on an H–R diagram; why is this description used and what is actually happening with the star?
7: On which edge of the main sequence band on an H–R diagram would the zero-age main sequence be?
8: How do stars typically “move” through the main sequence band on an H–R diagram? Why?
9: Certain stars, like Betelgeuse, have a lower surface temperature than the Sun and yet are more luminous. How do these stars produce so much more energy than the Sun?
10: Gravity always tries to collapse the mass of a star toward its centre. What mechanism can oppose this gravitational collapse for a star? During what stages of a star’s life would there be a “balance” between them?
11: Why are star clusters so useful for astronomers who want to study the evolution of stars?
12: Would the Sun more likely have been a member of a globular cluster or open cluster in the past?
13: Suppose you were handed two H–R diagrams for two different clusters: diagram A has a majority of its stars plotted on the upper left part of the main sequence with the rest of the stars off the main sequence; and diagram B has a majority of its stars plotted on the lower right part of the main sequence with the rest of the stars off the main sequence. Which diagram would be for the older cluster? Why?
14: Similar to the exercise above, referring to the same HR diagrams. Suppose you were handed two H–R diagrams for two different clusters: diagram A has a majority of its stars plotted on the upper left part of the main sequence with the rest of the stars off the main sequence; and diagram B has a majority of its stars plotted on the lower right part of the main sequence with the rest of the stars off the main sequence. Which diagram would more likely be the H–R diagram for an association?
15: The nuclear process for fusing helium into carbon is often called the “triple-alpha process.” Why is it called as such, and why must it occur at a much higher temperature than the nuclear process for fusing hydrogen into helium?
16: Pictures of various planetary nebulae show a variety of shapes, but astronomers believe a majority of planetary nebulae have the same basic shape. How can this paradox be explained?
17: Describe the two “recycling” mechanisms that are associated with stars (one during each star’s life and the other connecting generations of stars).
18: In which of these star groups would you mostly likely find the least heavy-element abundance for the stars within them: open clusters, globular clusters, or associations?
19: Explain how an H–R diagram of the stars in a cluster can be used to determine the age of the cluster.
20: Where did the carbon atoms in the trunk of a tree on your college campus come from originally? Where did the neon in the fabled “neon lights of Broadway” come from originally?
21: What is a planetary nebula? Will we have one around the Sun?
Thought Questions
22: Is the Sun on the zero-age main sequence? Explain your answer.
23: How are planetary nebulae comparable to a fluorescent light bulb in your classroom?
24: Which of the planets in our solar system have orbits that are smaller than the photospheric radius of Betelgeuse? You might remember from earlier in the Chapter that this radius = 5 x 1011 metres.
25: Would you expect to find an earthlike planet (with a solid surface) around a very low-mass star that formed right at the beginning of a globular cluster’s life? Explain.
26: In the H–R diagrams for some young clusters, stars of both very low and very high luminosity are off to the right of the main sequence, whereas those of intermediate luminosity are on the main sequence. Can you offer an explanation for that? Sketch an H–R diagram for such a cluster.
27: If the Sun were a member of the cluster NGC 2264, would it be on the main sequence yet? Why or why not?
28: If all the stars in a cluster have nearly the same age, why are clusters useful in studying evolutionary effects (different stages in the lives of stars)?
29: Suppose a star cluster were at such a large distance that it appeared as an unresolved spot of light through the telescope. What would you expect the overall colour of the spot to be if it were the image of the cluster immediately after it was formed? How would the colour differ after 1010 years? Why?
30: Suppose an astronomer known for joking around told you she had found a type-O main-sequence star in our Milky Way Galaxy that contained no elements heavier than helium. Would you believe her? Why?
31: Stars that have masses approximately 0.8 times the mass of the Sun take about 18 billion years to turn into red giants. How does this compare to the current age of the universe? Would you expect to find a globular cluster with a main-sequence turnoff for stars of 0.8 solar mass or less? Why or why not?
32: Automobiles are often used as an analogy to help people better understand how more massive stars have much shorter main-sequence lifetimes compared to less massive stars. Can you explain such an analogy using automobiles?
Figuring for Yourself
33: The text says a star does not change its mass very much during the course of its main-sequence lifetime. While it is on the main sequence, a star converts about 10% of the hydrogen initially present into helium (remember it’s only the core of the star that is hot enough for fusion). Look in earlier chapters to find out what percentage of the hydrogen mass involved in fusion is lost because it is converted to energy. By how much does the mass of the whole star change as a result of fusion? Were we correct to say that the mass of a star does not change significantly while it is on the main sequence?
34: The text explains that massive stars have shorter lifetimes than low-mass stars. Even though massive stars have more fuel to burn, they use it up faster than low-mass stars. You can check and see whether this statement is true. The lifetime of a star is directly proportional to the amount of mass (fuel) it contains and inversely proportional to the rate at which it uses up that fuel (i.e., to its luminosity).
Lifetime T = (M/L) in solar lifetimes.
If you want this number in years as opposed to solar lifetimes, since the lifetime of the Sun is about 1 x 1010 y, we have the following relationship:
T = (1 x 1010 years) x ( M / L)
where T is the lifetime of a main-sequence star, M is its mass measured in terms of the mass of the Sun, and L is its luminosity measured in terms of the Sun’s luminosity.
(Remember that the luminosity also depends on the mass of the star so as you will see later you can also write this as T = 1 / M 2.5 in solar lifetimes.)
- Explain in words why this equation works.
- Use the data from Chapter 18 which is reproduced below to calculate the ages of the main-sequence stars listed.
Characteristics of Main-Sequence Stars Spectral Type Mass (Sun = 1) Luminosity (Sun = 1) Temperature Radius (Sun = 1) O5 40 7 × 105 40,000 K 18 B0 16 2.7 × 105 28,000 K 7 A0 3.3 55 10,000 K 2.5 F0 1.7 5 7500 K 1.4 G0 1.1 1.4 6000 K 1.1 K0 0.8 0.35 5000 K 0.8 M0 0.4 0.05 3500 K 0.6 - Do low-mass stars have longer main-sequence lifetimes?
- Do you get the same answers as those in the table in the first section of this chapter? This table is reproduced for you below:
Lifetimes of Main-Sequence Stars Spectral Type Surface Temperature (K) Mass (Mass of Sun = 1)
Lifetime on Main Sequence (years) O5 54,000 40 1 million B0 29,200 16 10 million A0 9600 3.3 500 million F0 7350 1.7 2.7 billion G0 6050 1.1 9 billion K0 5240 0.8 14 billion M0 3750 0.4 200 billion
35: Use the equation from the question above which is
T = (1 x 1010 years) x ( M / L)
where T is the lifetime of a main-sequence star, M is its mass measured in terms of the mass of the Sun, and L is its luminosity measured in terms of the Sun’s luminosity.
Use the equation to estimate the approximate ages of the clusters in shown earlier in this chapter. Use the information in the figures to determine the luminosity of the most massive star still on the main sequence. Now use the data in the table below (reproduced from earlier in the textbook to estimate the mass of this star. Then calculate the age of the cluster. This method is similar to the procedure used by astronomers to obtain the ages of clusters, except that they use actual data and model calculations rather than simply making estimates from a drawing. How do your ages compare with the ages in the text?
| Characteristics of Main-Sequence Stars | ||||
|---|---|---|---|---|
| Spectral Type | Mass (Sun = 1) | Luminosity (Sun = 1) | Temperature | Radius (Sun = 1) |
| O5 | 40 | 7 × 105 | 40,000 K | 18 |
| B0 | 16 | 2.7 × 105 | 28,000 K | 7 |
| A0 | 3.3 | 55 | 10,000 K | 2.5 |
| F0 | 1.7 | 5 | 7500 K | 1.4 |
| G0 | 1.1 | 1.4 | 6000 K | 1.1 |
| K0 | 0.8 | 0.35 | 5000 K | 0.8 |
| M0 | 0.4 | 0.05 | 3500 K | 0.6 |
36: You can estimate the age of the planetary nebula shown in the planetary nebulae pictures earlier in this chapter. It is reproduced here as it is so beautiful.
The diameter of the nebula is about 0.8 light years, or more than five hundred times the diameter of our own solar system. The gas is expanding away from the star at a rate of about 40 km/s. Velocity = distance / time that gives time = distance / velocity. 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.
Remember that 1 light-year = 9.46 x 1012 km = 9.46 x 1015 metres
Remember that 1 year = 3.15 x 107 seconds
37: If star A has a core temperature T, and star B has a core temperature 3T, how does the rate of fusion of star A compare to the rate of fusion of star B? Bigger, smaller or about the same? Remember the law of conservation of energy.
38: Remember from the text that the equation that relates temperate and rate of fusion depends on Wein’s Law.
Star Temperature and Rate of Fusion If a star’s temperature were to double, by what factor would its rate of fusion increase?
Solution Since the rate of fusion (like temperature) goes up to the fourth power, it would increase by a factor of 24, or 16 times.
Check Your Learning If the rate of fusion of a star increased 256 times, by what factor would the temperature increase?
If star A has a core temperature T, and star B has a core temperature 5T, how does the rate of fusion of star A compare to the rate of fusion of star B in numbers?
Asnwers to the Figuring it Yourself Questions
35) You have already been given the answers in the question. Keep scrolling.
36) distance = 0.8 light-years = 8 x 10 15 m so time = distance / velocity = 2 x 10 11 seconds = 6000 years
37) It has to be bigger. The law of conservation of energy means that if the core temperate is hotter, that energy has to come from somewhere, in this case the fusion of hydrogen into helium or E=mc2, so the rate of fusion has to be bigger.
38) 1/54 = 625