3. a) Explain how it is possible for the core of a red giant to contract at the same time that its outer layers expand. b) What is the asymptotic giant branch? Where is it located on a Hertzsprung-Russell (H-R) diagram? Describe how asymptotic giant branch stars differ from main-sequence stars and stars on the red giant branch.
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- 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.You discover a binary star system in which one member is a 15 solar-mass main-sequence star and the other star is a 10 solar-mass giant. Why should you be surprised, at least at first? A. It doesn't make sense to find a giant in a binary star system. B. The two stars in a binary system should both be at the same point in stellar evolution; that is, they should either both be main-sequence stars or both be giants. C. The two stars should be the same age, so the more massive one should have become a giant first. D. The odds of ever finding two such massive stars in the same binary system are so small as to make it inconceivable that such a system could be discovered. E. A star with a mass of 15 solar-mass is too big to be a main-sequence star.Based on what you know about main-sequence stars, select all of the correct statements from the following list. 1. Since the interiors of stars cannot be observed, there are no theories about their structure. 2. More massive stars are hotter and brighter. 3. The weight of a star must be balanced by internal pressure. 4. More massive stars live longer; they take longer to use up all their energy. 5. Stars change position on the main sequence throughout their lives. 6. Outward energy flow in a star is by conduction only.
- For 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.Astronomers studying regions like the Orion Giant Molecular Cloud have observed that a wave of star formation can move through them over many millions of years. What sustains such a wave of star formation in a giant molecular cloud? A. radio waves from complex molecules move slowly through the cloud, causing stars to form B. when a group of stars form, they remove so much material from the cloud that only a big empty place is left, into which new matter from other clouds falls, making more stars C. when giant molecular clouds collide with each other, they do so not just once, but many times D. the dust in these clouds is so heavy, it is always settling inward toward the cloud's center causing star formation in its wakeBased on what you learned about stellar structure and how stars maintain their stability, select all of the correct statements from the following list. 1. The weight pressing down on a layer of gas in a star is balanced by the pressure in the gas. 2. The interior of the lowest-mass stars transfers energy mostly through convection. 3. Energy in a star flows from the core to the surface. 4. More massive stars produce energy with the proton-proton cycle. 5. Less massive stars produce energy with the CNO cycle. 6. Conduction is an important method of energy transport in stars. 7. Stars are hotter in their cores than on their surfaces.
- Which portion of the EM spectrum is best for understanding the giant Molecular Clouds from which stars are born? Far infrared GXUVIR a. FAR IR b. VISIBLE OC. NEAR IR Od. Molecular Clouds are not shown in any of them Oe. All show the clouds equally well Visible wwwwwwww GXUVR Near infrared. www GXUVIRBased 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.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 HR diagram.
- 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.The evolutionary track for a star of 1 solar mass remains nearly vertical in the HR diagram for a while (see Figure 21.12). How is its luminosity changing during this time? Its temperature? Its radius? Figure 21.12 Evolutionary Tracks for Contracting Protostars. Tracks are plotted on the HR diagram to show how stars of different masses change during the early parts of their lives. The number next to each dark point on a track is the rough number of years it takes an embryo star to reach that stage (the numbers are the result of computer models and are therefore not well known). Note that the surface temperature (K) on the horizontal axis increases toward the left. You can see that the more mass a star has, the shorter time it takes to go through each stage. Stars above the dashed line are typically still surrounded by infalling material and are hidden by it.A group of graduate students, bored during a cloudy night at a the observatory, begin to make bets about the time different stars will take to evolve. If they have a cluster of stars which were all born roughly the same time, and want to know which star will become a red giant first, which of the following stars should they bet on? a. a star that would type O on the main sequence star b. a star about 1/2 the mass of our sun c. a star about 8% the mass of our sun d. all stars reach the red giant stage in roughly the same number of years
