Astronomy
1st Edition
ISBN: 9781938168284
Author: Andrew Fraknoi; David Morrison; Sidney C. Wolff
Publisher: OpenStax
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Textbook Question
Chapter 22, Problem 27E
If the Sun were a member of the cluster NGC 2264, would it be on the main sequence yet? Why or why not?
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The Orion Nebula is about 20 light-years (20 × 1018 cm) across, enclosing a roughly spherical area with a volume of 4.19 × 1057 cm3. Calculate the number of 0.1 solar mass stars that might be formed in such a nebula. Assume that the nebula has a density of 1000 atoms/cm3.
If the RR Lyrae stars in a globular cluster have average apparent magnitudes of +19, how far away (in pc) is the cluster? (Hints: See the following figure, and use the magnitude-distance formula: d = 10(mv - My+5)/5.)
Туре
(Classical)
Cepheids
104
103
Туре II
Cepheids
102
RR Lyrae stars
0.3
1
10
30
100
Pulsation perlod (days)
pc
Absolute magnitude
Luminosity, L L.
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.)
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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- You can use the equation in Exercise 22.34 to estimate the approximate ages of the clusters in Figure 22.10, Figure 22.12, and Figure 22.13. 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 Table 18.3 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? Figure 22.10 NGC 2264 HR Diagram. Compare this HR diagram to that in Figure 22.8; although the points scatter a bit more here, the theoretical and observational diagrams are remarkably, and satisfyingly, similar. Figure 22.12 Cluster M41. (a) Cluster M41 is older than NGC 2264 (see Figure 22.10) and contains several red giants. Some of its more massive stars are no longer close to the zero-age main sequence (red line). (b) This ground-based photograph shows the open cluster M41. Note that it contains several orange-color stars. These are stars that have exhausted hydrogen in their centers, and have swelled up to become red giants. (credit b: modification of work by NOAO/AURA/NSF) Figure 22.13 HR Diagram for an Older Cluster. We see the HR diagram for a hypothetical older cluster at an age of 4.24 billion years. Note that most of the stars on the upper part of the main sequence have turned off toward the red-giant region. And the most massive stars in the cluster have already died and are no longer on the diagram. Characteristics of Main-Sequence Starsarrow_forwardIn the HR 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 HR diagram for such a cluster.arrow_forwardWould the Sun more likely have been a member of a globular cluster or open cluster in the past?arrow_forward
- According to the text, a star must be hotter than about 25,000 K to produce an H II region. Both the hottest white dwarfs and main-sequence O stars have temperatures hotter than 25,000 K. Which type of star can ionize more hydrogen? Why?arrow_forwardWhy do nebulae near hot stars look red? Why do dust clouds near stars usually look blue?arrow_forward
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