21st Century Astronomy
6th Edition
ISBN: 9780393428063
Author: Kay
Publisher: NORTON
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Chapter 18, Problem 15QP
To determine
Does the current model of long duration GRB includes.
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Why 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 c
If 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 bang
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
Chapter 18 Solutions
21st Century Astronomy
Ch. 18.1 - Prob. 18.1CYUCh. 18.2 - Prob. 18.2CYUCh. 18.3 - Prob. 18.3CYUCh. 18.4 - Prob. 18.4CYUCh. 18 - Prob. 1QPCh. 18 - Prob. 2QPCh. 18 - Prob. 3QPCh. 18 - Prob. 4QPCh. 18 - Prob. 5QPCh. 18 - Prob. 6QP
Ch. 18 - Prob. 7QPCh. 18 - Prob. 8QPCh. 18 - Prob. 9QPCh. 18 - Prob. 10QPCh. 18 - Prob. 11QPCh. 18 - Prob. 12QPCh. 18 - Prob. 13QPCh. 18 - Prob. 14QPCh. 18 - Prob. 15QPCh. 18 - Prob. 16QPCh. 18 - Prob. 17QPCh. 18 - Prob. 18QPCh. 18 - Prob. 19QPCh. 18 - Prob. 20QPCh. 18 - Prob. 21QPCh. 18 - Prob. 22QPCh. 18 - Prob. 23QPCh. 18 - Prob. 24QPCh. 18 - Prob. 25QPCh. 18 - Prob. 26QPCh. 18 - Prob. 27QPCh. 18 - Prob. 28QPCh. 18 - Prob. 29QPCh. 18 - Prob. 30QPCh. 18 - Prob. 31QPCh. 18 - Prob. 32QPCh. 18 - Prob. 33QPCh. 18 - Prob. 34QPCh. 18 - Prob. 35QPCh. 18 - Prob. 36QPCh. 18 - Prob. 37QPCh. 18 - Prob. 38QPCh. 18 - Prob. 39QPCh. 18 - Prob. 40QPCh. 18 - Prob. 41QPCh. 18 - Prob. 42QPCh. 18 - Prob. 43QPCh. 18 - Prob. 44QPCh. 18 - Prob. 45QP
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Need a deep-dive on the concept behind this application? Look no further. Learn more about this topic, physics and related others by exploring similar questions and additional content below.Similar questions
- 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.arrow_forwardAs a white dwarf cools, its radius will not change because a. pressure resulting from nuclear reactions in a shell just below the surface keeps it from collapsing. b. pressure does not depend on temperature for a white dwarf because the electrons are degenerate. c. pressure does not depend on temperature because the white dwarf is too hot. d. pressure does not depend on temperature because the star has exhausted all its nuclear fuels. e. material accreting onto it from a companion maintains a constant radius.arrow_forwardThe diagram below shows an H-R diagram with life track of a 1-solar-mass star, with various stages labeled A through E. Temperature What will happen to the star after stage E? A. It will gain mass until it collapses under its own weight. B. It will begin burning carbon in its core. C. It will explode in a supernova. D. It will collapse to make a neutron star. E. It will eject a planetary nebula. Luminosity →arrow_forward
- A Type Ia Supernova is an example of a: a. Parallax object b. Moving cluster object c. Standard ruler object d. Standard candle objectarrow_forward24 If the Temperature of the core of a supernova is 3200 x 1023 K, what should be the average translational kinetic energy of the particles moving inside this supernov (Boltzmann's constant = 1.38 x 10-23 J/K) Type your answer...arrow_forwardA main sequence star of mass, M, and radius, R, collapses to a white dwarf star with a radius 1.0% as big as the original star. If ω is the angular velocity of the original star, what is the angular velocity of the white dwarf star? Approximate the star to be a uniform solid sphere. a. 20,000ω b. 10,000ω c. 50,000ω d. 1,000ω e. 5,000ωarrow_forward
- 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_forward4. What is the upper limit of a brown dwarf’s size? a. no upper limit b. 0.50 solar masses c. 0.10 solar masses d. 0.08 solar masses e. less than 0.08 solar massesOn this one, I feel like E is the answer because the book mentions a red dwarf that is .08 solar masses in the section about brown dwarfs. I just want to be sure that D is not what they are looking for. (I've asked the professor, but I am not having any luck getting in touch with him.)arrow_forwardGM What is the orbital period of a bit of matter in an accretion disk that is located 3 x 105 km from a 29 M. black hole? (Hint: Use the circular orbit velocity formula, V. = Varrow_forward
- The chemical abundance of population I stars a. indicates that they were formed before the population II stars. b. indicates that the material they formed from had been enriched with material from supernovae. c. indicates that they contain very few heavy metals compared to halo stars. d. depends on the temperature of the star. e. depends on the mass of the star.arrow_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_forwardThe orbit of the binary pulsar PSR 1936+16, studied by Taylor and Hulse, a. is so small that the orbital period is smaller than the pulsar period. b. is growing smaller, presumably by emitting gravitational waves. c. provides evidence that it is being orbited by at least 6 planets the size of Jupiter. d. shows large changes each time an X ray burst is emitted from the system. e. contains a white dwarf and a black hole.arrow_forward
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