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 14, Problem 7TY
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As a cluster of stars begins to age, which type of star in the cluster will move off the main sequence of the H-R diagram first?
1)
all the stars in a cluster are born at the same time; so they will all move off the main sequence at the same time, as they evolve
2)
G type stars, like our Sun
3)
M type stars, which are the coolest
4)
the lowest mass stars, which have the least amount of fuel for fusion
5)
the O and B type stars
Which of the following statements is wrong?
A. A main-sequence star is cooler and brighter than it was as a protostar.
B. Carbon fusion occurs in high-mass stars but not in low-mass stars because the cores of low-mass stars never contain significant amounts of carbon.
C. when a main-sequence star exhausts its core hydrogen fuel supply, the core shrinks while the rest of the star expands.
D. After a supernova explosion, the remains of the stellar core will be either a neutron star or a black hole.
Place the following events in the formation of stars in the proper chronological
sequence, with the oldest first and the youngest last.
w. the gas and dust in the nebula flatten to a disk shape due to gravity
and a steadily increasing rate of angular rotation
x. a star emerges when the mass is great enough and the temperature is
high enough to trigger thermonuclear fusion in the core
y. the rotation of the nebular cloud increases as gas and dust
concentrates by gravity within the growing protostar in the center
z. some force, perhaps from a nearby supernova, imparts a rotation to a
nebular cloud
y, then z, then w, then x
z, then y, then w, then x
w, then y, then z, then x
z, then x, then w, then y
x, then z, then y, then w
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Chapter 14 Solutions
Loose Leaf For Explorations: Introduction To Astronomy
Ch. 14 - Prob. 1QFRCh. 14 - Prob. 2QFRCh. 14 - Prob. 3QFRCh. 14 - Prob. 4QFRCh. 14 - Prob. 5QFRCh. 14 - Prob. 6QFRCh. 14 - Prob. 7QFRCh. 14 - Prob. 8QFRCh. 14 - Prob. 9QFRCh. 14 - Prob. 10QFR
Ch. 14 - Prob. 11QFRCh. 14 - Prob. 12QFRCh. 14 - Prob. 13QFRCh. 14 - Prob. 14QFRCh. 14 - Prob. 15QFRCh. 14 - Prob. 16QFRCh. 14 - Prob. 17QFRCh. 14 - Prob. 18QFRCh. 14 - Prob. 19QFRCh. 14 - Prob. 20QFRCh. 14 - Prob. 21QFRCh. 14 - Prob. 22QFRCh. 14 - Prob. 23QFRCh. 14 - Prob. 24QFRCh. 14 - Prob. 1TQCh. 14 - Prob. 2TQCh. 14 - Prob. 3TQCh. 14 - Prob. 5TQCh. 14 - Prob. 7TQCh. 14 - Prob. 8TQCh. 14 - Prob. 9TQCh. 14 - Prob. 10TQCh. 14 - Prob. 1PCh. 14 - Prob. 2PCh. 14 - Prob. 3PCh. 14 - Prob. 4PCh. 14 - Prob. 5PCh. 14 - Prob. 6PCh. 14 - Prob. 7PCh. 14 - Prob. 8PCh. 14 - Prob. 9PCh. 14 - Prob. 1TYCh. 14 - Prob. 2TYCh. 14 - Prob. 3TYCh. 14 - Prob. 4TYCh. 14 - Prob. 5TYCh. 14 - Prob. 6TYCh. 14 - Prob. 7TYCh. 14 - Prob. 8TYCh. 14 - Prob. 9TYCh. 14 - Prob. 10TYCh. 14 - Prob. 11TY
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- The theory that the collapse of a massive star’s iron core produces neutrinos was supported by a. the size and structure of the Crab nebula. b. laboratory measurements of the mass of the neutrino. c. the brightening of supernovae a few days after they are first visible. d. underground counts from solar neutrinos. e. the detection of neutrinos from the supernova of 1987.arrow_forwardThe two types of cycles proposed in the stars for fusion are ________ a) p-p cycle and p-e cycle b) p-p cycle and C-N cycle c) p-p cycle and p-C cycle d) p-p cycle and p-N cyclearrow_forwardThe 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?arrow_forward
- Look at the four stages shown in Figure 21.8. In which stage(s) can we see the star in visible light? In infrared radiation? Figure 21.8 Formation of a Star. (a) Dense cores form within a molecular cloud. (b) A protostar with a surrounding disk of material forms at the center of a dense core, accumulating additional material from the molecular cloud through gravitational attraction. (c) A stellar wind breaks out but is confined by the disk to flow out along the two poles of the star. (d) Eventually, this wind sweeps away the cloud material and halts the accumulation of additional material, and a newly formed star, surrounded by a disk, becomes observable. These sketches are not drawn to the same scale. The diameter of a typical envelope that is supplying gas to the newly forming star is about 5000 AU. The typical diameter of the disk is about 100 AU or slightly larger than the diameter of the orbit of Pluto.arrow_forwardWhat is a planetary nebula? Will we have one around the Sun?arrow_forwardDescribe what happens when a star forms. Begin with a dense core of material in a molecular cloud and trace the evolution up to the time the newly formed star reaches the main sequence.arrow_forward
- Arrange the following stars in order of their evolution: A. A star with no nuclear reactions going on in the core, which is made primarily of carbon and oxygen. B. A star of uniform composition from center to surface; it contains hydrogen but has no nuclear reactions going on in the core. C. A star that is fusing hydrogen to form helium in its core. D. A star that is fusing helium to carbon in the core and hydrogen to helium in a shell around the core. E. A star that has no nuclear reactions going on in the core but is fusing hydrogen to form helium in a shell around the core.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_forwardYou 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_forward
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