Hertzsprung-Russell DiagramBhue or blue whiteWhiteVellowRed-orangeRedORigelSuperglantsBeteignuneMain SequenceAldebaranGlantsSunAlpho Centour BSinus BWhite Dwarfs50.00020,00010,000Surface Temperature ('C)6.0005,0003.000Most of the stars shown on the diagram are classified as which type of star?O white dwarfO main sequenceO red giantO super giantBrightnessIncreasing-

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Hertzsprung-Russell Diagram Bhe or bhue white White Vellow Red orange Red ORigel Superglants Betelgrne Main Sequence Aldebaran Glants Alpho Centaur e Sinus 8 White Dwarfs 30.000 20,000 10,000 6,000 Surface Temperature ('C) 5,000 3,000 Most of the stars shown on the diagram are classified as which type of star? O white dwarf O main sequence O red giant O super giant Brightness busea

Hertzsprung-Russell Diagram Bhe or bhue white White Vellow Red orange Red ORigel Superglants Betelgrne Main Sequence Aldebaran Glants Alpho Centaur e Sinus 8 White Dwarfs 30.000 20,000 10,000 6,000 Surface Temperature ('C) 5,000 3,000 Most of the stars shown on the diagram are classified as which type of star? O white dwarf O main sequence O red giant O super giant Brightness busea

Stars and Galaxies (MindTap Course List)

10th Edition

ISBN:9781337399944

Author:Michael A. Seeds

Publisher:Michael A. Seeds

Chapter12: Stellar Evolution

Section: Chapter Questions

Problem 7P

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Why are titanium oxide features visible in the spectra of only the coolest stars? Pls explain well
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Dust was originally discovered because the stars in certain clusters seemed to be fainter than expected. Suppose a star is behind a cloud of dust that dims its brightness by a factor of 100. Suppose you do not realize the dust is there. How much in error will your distance estimate be? Can you think of any measurement you might make to detect the dust?
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). Since the lifetime of the Sun is about 1010 y, we have the following relationship: T=1010MLy 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. A. Explain in words why this equation works. B. Use the data in Table 18.3 to calculate the ages of the main-sequence stars listed. C. Do low-mass stars have longer main-sequence lifetimes? D. Do you get the same answers as those in Table 22.1?
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