The Cosmic Perspective Fundamentals (2nd Edition)
2nd Edition
ISBN: 9780133889567
Author: Jeffrey O. Bennett, Megan O. Donahue, Nicholas Schneider, Mark Voit
Publisher: PEARSON
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Chapter 10, Problem 15SEQ
To determine
To Predict:
The result of x-ray binary star eventually feeding 3 solar masses of matter into the neutron star's accretion disk.
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What kind of star is most likely to become a white-dwarf supernova?
A. a star like our Sun
B. a white dwarf star with a red giant binary companion
C. a pulsar
D. an O star
Is the answer B?
For D, as the surface temperature of a star would change over time so spectral type cannot tell us about the fate of the stars?
2GM
What is the escape velocity (in km/s) from the surface of a 1.1 Mo neutron star? From a 3.0 M, neutron star? (Hint: Use the formula for escape velocity, V. =
make sure to express quantities in units of meters, kilograms, and seconds. Assume a neutron star
has a radius of 11 km and assume the mass of the Sun is 1.99 x 1030 kg.)
1.1 Me neutron star
km/s
3.0 M. neutron star
km/s
Astronomers us the P-Cygni line features in a spectrum of a supernova to...
Select one alternative:
...measure the velocity of the supernova ejecta.
...to measure the rotation speed of the star that exploded.
...measure the composition of the supernova ejecta more accurately than with other lines.
...to measure the mass of the neutron star or black hole formed in the supernova.
Chapter 10 Solutions
The Cosmic Perspective Fundamentals (2nd Edition)
Ch. 10 - Prob. 1QQCh. 10 - Prob. 2QQCh. 10 - Prob. 3QQCh. 10 - Prob. 4QQCh. 10 - Prob. 5QQCh. 10 - Prob. 6QQCh. 10 - Prob. 7QQCh. 10 - Choose the best answer to each of the following....Ch. 10 - Prob. 9QQCh. 10 - Choose the best answer to each of the following....
Ch. 10 - Prob. 11QQCh. 10 - Prob. 12QQCh. 10 - Explain all answers clearly, with complete...Ch. 10 - Explain all answers clearly, with complete...Ch. 10 - Prob. 15SEQCh. 10 - Prob. 16SEQCh. 10 - Prob. 17SEQCh. 10 - Prob. 18SEQCh. 10 - Prob. 19SEQCh. 10 - Explain all answers clearly, with complete...
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- A. Estimate the surface gravity of a neutron star with R = 10 km and M = 2M. . B. Determine the density of such a neutron star in g/cm³. C. How much would a teaspoon (5 cm³) of this neutron star weigh on Earth? This material is known as neutronium. Give your answer in pounds. D. Which would be heavier: a teaspoon of neutronium weighed on Earth, or a teaspoon of water weighed on the surface of a neutron star?arrow_forwardIf a star is to eventually form a stellar black hole at any point in its life cycle what must happen? A. Gravity must be strong enough to compress all its material to be smaller than its schwartzchild radius B. it must pass by a supermassive black hole and tidal forces will do the rest C. Gravity must expand it so it can over power the nuclear forces that compress it and keep it from exploding by giving off all its heat D. A star will always have the same mass and radius and the only black holes that exist are ones that have existed shortly after the big bangarrow_forwardWhat keeps a neutron star from collapsing?a. the thermal pressure resulting from nuclear fusion in its core; b. the degenerate neutron gas pressure;c. the degenerate electron gas pressure;d. the convectionarrow_forward
- 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?arrow_forwardWhere in the Galaxy would you expect to find Type II supernovae, which are the explosions of massive stars that go through their lives very quickly? Where would you expect to find Type I supernovae, which involve the explosions of white dwarfs?arrow_forwardWhat is the escape velocity (in km/s) from the surface of a 1.1 M. neutron star? From a 3.0 M. neutron star? (Hint: Use the formula for escape velocity, V̟ = V 2GM ; make sure to express quantities in units of meters, kilograms, and seconds. Assume a neutron star has a radius of 11 km and assume the mass of the Sun is 1.99 x 1030 kg.) 1.1 M neutron star km/s 3.0 M. neutron star km/s If a neutron star has a radius of 12 km and a temperature of 8.0 x 10° K, how luminous is it? Express your answer in watts and also in solar luminosity units. (Hint: Use the relation Use 5,800 K for the surface temperature of the Sun. The luminosity of the Sun is 3.83 x 1026 w.) luminosity in watts luminosity in solar luminosity unitsarrow_forward
- Which of the following statements about various stages of core nuclear burning (hydrogen, helium, carbon, etc.) in a high- mass star is not true? A. As each stage ends, the core shrinks and heats further. B. Each successive stage creates an element with a higher atomic number and atomic mass number. C. As each stage ends, the reactions that occurred in previous stages continue in shells around the core. D.Each successive stage lasts for approximately the same amount of time.arrow_forwardIndicate whether the following are properties of Type Ia or Type II supernovae. (Select 1-Type Ia, 2-Type II. If the first is 1 and the rest 2, enter 12222222). A) Can occur in a very old star cluster. B) Can only occur in a binary system. C) The spectrum shows strong Hydrogen lines D) Produces very heavy elements like Uranium during the explosion. F) Could completely explode and leave no remnant behind. Supernovae of this type have the same peak luminosity.arrow_forward4arrow_forward
- 5arrow_forwardWhy don’t all supernova remnants contain pulsars? a. All supernova remnants do contain pulsars. b. Some supernova explosions form white dwarfs instead of the neutron stars necessary for pulsars. c. Pulsars slow down and quit producing the pulses before the supernova remnant dissipates. d. The pulsar may be tipped so that the beams do not sweep past Earth. e. b and carrow_forwardWhich of the following is least reasonable regarding novae and supernovae? Group of answer choices A type I (carbon-detonation) supernova results when a white dwarf in a binary system absorbs enough mass from its companion to push it over the Chandrasekhar limit. A type II supernova results from any supermassive star at the end of its life, when it runs out of fusion energy and collapses. A nova can occur multiple times in a binary system. If a white dwarf in a binary system absorbs enough mass to go beyond the Chandrasekhar limit, the white dwarf explodes as a supernova. The reason a type I supernova does not produce hydrogen lines is that the explosion originates from a stellar core (white dwarf), where hydrogen has already fused to produce heavier elements (so there is no longer any hydrogen). More supernovae are observed in the Milky Way because they are much closer to us than those in other galaxies.arrow_forward
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