Concept explainers
a
To Evaluate: The following prediction. “Type O stars have shorter lives than type G stars”.
b
To Evaluate: The following prediction.
“Type K supergiant stars produce iron before they explode as supernovae.”
c
To Evaluate: The following prediction:
Type F stars become much more luminous near the ends of their lives than they were as main-sequence stars.
d
To Evaluate: The following prediction:
“Type O stars do not become more luminous near the ends of their lives but do become redder.”
e
To Evaluate: The following prediction:
“Type M stars should have longer lives than type K stars.”
f
To Evaluate: The following prediction:
“Stars similar to Sun reach a maximum size of about 100 solar radii during the red giant stage.”
g
To Evaluate: The following prediction:
“Type K main sequence stars will become red giants when their cores run out of hydrogen.”
h
To Evaluate: The following prediction:
“Some stars become white dwarfs at the ends of their lives.”
i
To Evaluate: The following prediction:
“White dwarfs cool with time but do not change much in radius.”
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Check out a sample textbook solutionChapter 13 Solutions
ESSENTIAL COSMIC PERS.-W/MASTER.ACCESS
- Topic: Life cycle of stars Q. What color are the hottest stars? What color are the coolest stars?arrow_forwardThe sketch below shows an H-R diagram for a star cluster. Consider the star to which the arrow points. How is it currently generating energy? Temperature A. by hydrogen shell burning around an inert helium core B. by gravitational contraction C. by core hydrogen fusion D.by core helium fusion combined with hydrogen shell burning E. by both hydrogen and helium shell burning around an inert carbon core Luminosity -→arrow_forwardBased on what you learned about stellar evolution, select all of the correct statements from the following list. 1. The period of some Cepheid variables actually changes. 2. When getting dimmer, variable stars are releasing energy; when getting brighter they are storing energy. 3. variable stars are expanding and contracting 4. despite their variability, variable stars stay in a specific position on the H-R diagram. 5. A changing period in a Cepheid variable means that the size of the star is changing and that the star is therefore evolving. 6. Only stars on the instability strip are variable. 7. More massive stars will vary their brightness more quickly.arrow_forward
- Cluster Sizes. An open cluster is a collection of 10 to 1000 stars in a region about 25 pc in diameter. About how far apart are the stars in an open cluster in units of pc? (Hints: What share of the cluster's volume belongs to a single 4 Tr. Use the cited value for the maximum number of stars in your calculation.) star? The volume of a sphere is pc.arrow_forwardChoose the correct statements concerning spectral classes of stars. (Give ALL correct answers, i.e., B, AC, BCD...) A) Neutral hydrogen lines dominate the spectrum for stars with temperatures around 10,000 K because a lot of the hydrogen is in the n=2 level. B) Hydrogen lines are weak in type O-stars because most of it is completely ionized. C) Oh Be A Fine Guy/Girl Kiss Me, is a mnemonic for remembering spectral classes. D) The spectral sequence has recently been expanded to include L, T, and Y classes. E) K-stars are dominated by lines from ionized helium because they are so hot. F) The spectral types of stars arise primarily as a result of differences in temperature.arrow_forwardPlace 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 MacBook Air on .H. O O O Oarrow_forward
- Topic: Life Cycle of Stars Q. Describe what would our Sun look like from Earth if it was a massive star? Pls answer in 2-3 sentences. Thank You!arrow_forwardFor each statement concerning main sequence stars, select T True, F False, G Greater than, L Less than, or E Equal to. A) The surface temperature of a O type star is .... than a K type star. B) On the main sequence, the mass of a O type star is .... than a F type star. C) On the main sequence, a M type star's life is .... than a G type star. D) The surface temperature of our Sun is .... than the surface temperature of Sirius. E) When stars start hydrogen burning, thier mass determines where they are on the main sequence. F) Based on the relative lifes of M and G type stars we expect the number of M stars to be .... than the number of G type stars.arrow_forwardChoose the correct statements concerning spectral classes of stars. (Give ALL correct answers, i.e., B, AC, BCD...) A) K-stars are dominated by lines from ionized helium because they are so hot. B) Oh Be A Fine Guy/Girl Kiss Me, is a mnemonic for remembering spectral classes. C) The spectral sequence has recently been expanded to include L, T, and Y classes. D) Hydrogen lines are weak in type O-stars because most of it is completely ionized. E) Neutral hydrogen lines dominate the spectrum for stars with temperatures around 10,000 K because a lot of the hydrogen is in the n=2 level. F) The spectral types of stars arise primarily as a result of differences in chemical composition.arrow_forward
- All massive main sequence stars reside in clouds of glowing gas. The four powerful stars in the center of the Orion Nebula are good examples. Lower mass stars like the Sun generally don't have clouds of gas around them. a. Why do powerful stars reside in gas clouds? b. What is making the gas glow exactly? For the last question, refer to the surface temperature of these stars, and to Wien's Law.arrow_forwardWe can estimate the masses of most of the stars in Appendix J from the mass-luminosity relationship in Figure 18.9. However, remember this relationship works only for main sequence stars. Determine which of the first 10 stars in Appendix J are main sequence stars. Use one of the figures in this chapter. Make a table of stars’ masses. Figure 18.9 Mass-Luminosity Relation. The plotted points show the masses and luminosities of stars. The three points lying below the sequence of points are all white dwarf stars.arrow_forwardMatch each characteristic below of a one-solar-mass star to its appropriate phase. Answer M for Main-sequence Star, or P for Protostar. If the first is M and the rest P, enterMPPPPPP). A) energy generated by nuclear fusion B) pressure and gravity are NOT precisely balanced. C) surface radiates energy at same rate that core generates energy D) radius much larger than the Sun E) energy generated by gravitational contraction F) lasts about 10 billion years G) luminosity much greater than the Sunarrow_forward