Loose Leaf For Explorations: Introduction To Astronomy
9th Edition
ISBN: 9781260432145
Author: Thomas T Arny, Stephen E Schneider Professor
Publisher: McGraw-Hill Education
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Chapter 15, Problem 2TY
To determine
The correct option which must be satisfied for a white dwarf or a neutron star to shrink.
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Let's compare the acceleration due to gravity at the surface of a Sun-like star to a white dwarf of similar mass. We know that the force of gravity comes from F= G*m_1*m_2/r^2 and that F = m * a from some of Newton's laws. As such, we know that the acceleration due to gravity is given by a_g = G*m/r^2.
With that in mind, let's say that we have a white dwarf star is approximately the size of the Earth which is 1/100 radius of the Sun (0.01 R Sun) and that the white dwarf has a mass that is approximately half the mass of the Sun (0.5 M_Sun). What is the ratio of the acceleration due to gravity at the surface of the white dwarf star (aka the surface gravity) compared to the surface gravity of the Sun-like star (assume its mass is 1 M_sun and radius is 1 R_Sun).?
QUESTION 21
In a Type Ia supernova, the cause of the violent outburst is:
1)
the sudden emission of a shell of stellar material from a dying low-mass star
2)
the collapse of a very massive protostar to the main sequence
3)
an enormous release of neutrinos during a sudden episode of hydrogen fusion
4)
the transfer of so much mass from a companion star that a white dwarf goes "over the limit" and collapses, causing an enormous amount of sudden fusion
5)
two neutron stars colliding with each other
What is the escape velocity at the surface of a typical neutron star?
Chapter 15 Solutions
Loose Leaf For Explorations: Introduction To Astronomy
Ch. 15 - Prob. 1QFRCh. 15 - Prob. 2QFRCh. 15 - Prob. 3QFRCh. 15 - Prob. 4QFRCh. 15 - Prob. 5QFRCh. 15 - Prob. 6QFRCh. 15 - Prob. 7QFRCh. 15 - Prob. 8QFRCh. 15 - Prob. 9QFRCh. 15 - Prob. 10QFR
Ch. 15 - Prob. 11QFRCh. 15 - Prob. 12QFRCh. 15 - Prob. 13QFRCh. 15 - What is nonthermal radiation?Ch. 15 - What happens when a gravitational wave moves? What...Ch. 15 - What is a black hole? Are they truly black? What...Ch. 15 - Prob. 17QFRCh. 15 - Prob. 18QFRCh. 15 - Prob. 19QFRCh. 15 - Prob. 20QFRCh. 15 - Prob. 1TQCh. 15 - Prob. 2TQCh. 15 - Prob. 3TQCh. 15 - Prob. 5TQCh. 15 - Prob. 6TQCh. 15 - Prob. 7TQCh. 15 - Prob. 8TQCh. 15 - Suppose you jumped into a black hole feet first....Ch. 15 - Prob. 10TQCh. 15 - Prob. 1PCh. 15 - Prob. 2PCh. 15 - Prob. 3PCh. 15 - Prob. 4PCh. 15 - Prob. 5PCh. 15 - Prob. 6PCh. 15 - Prob. 7PCh. 15 - Prob. 8PCh. 15 - Prob. 9PCh. 15 - Prob. 10PCh. 15 - Prob. 11PCh. 15 - Prob. 12PCh. 15 - Prob. 1TYCh. 15 - Prob. 2TYCh. 15 - Prob. 3TYCh. 15 - Prob. 4TYCh. 15 - Prob. 5TYCh. 15 - Prob. 6TYCh. 15 - What evidence leads astronomers to believe that...Ch. 15 - (15.3) The Schwarzschild radius of a body is (a)...Ch. 15 - Prob. 9TYCh. 15 - Prob. 10TY
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- How would the spectra of a type II supernova be different from a type Ia supernova? Hint: Consider the characteristics of the objects that are their source.arrow_forwardA light of wavelength 620 nm is emitted from the following four places. What wavelength is observed for this light by an observer a long distance away? (The objects are not moving with respect to the observer) The surface of a 0.84 solar mass white dwarf that has a radius of 708000 km: ? The surface of a 2.52 solar mass neutron star that has a radius of 14.2 km: 2 Schwarzschild radii from a 20 solar mass black hole: ? 1.048 Schwarzschild radii from a 20 solar mass black hole: ?arrow_forwardA star has initially a radius of 780000000 m and a period of rotation about its axis of 22 days. Eventually it changes into a neutron star with a radius of only 25000 m and a period of 0.1 s. Assuming that the mass has not changed, find Assume a star has the shape of a sphere. (Suggestion: do it with formula first, then put the numbers in) [Recommended time : 5-8 minutes] (a) the ratio of initial to final angular momentum (Li/Lf) a. 1.85E+16 b. 51.2 c. 0.0195 d. 5.4E-17 (b) the ratio of initial to final kinetic energy a. 2.84E-24 b. 371000 c. 2.69E-6 d. 3.52E+23arrow_forward
- A star has initially a radius of 680000000 m and a period of rotation about its axis of 26 days. Eventually it changes into a neutron star with a radius of only 40000 m and a period of 0.2 s. Assuming that the mass has not changed, find Assume a star has the shape of a sphere. (Suggestion: do it with formula first, then put the numbers in) [Recommended time : 5-8 minutes] (a) the ratio of initial to final angular momentum (Li/Lf) Oa. 3.25E+15 Ob. 25.7 Oc. 0.0389 Od. 3.08E-16 (b) the ratio of initial to final kinetic energy Oa. 2.74E-23 Ob. 437000 Cc. 2.29E-6 FUJITSUarrow_forwardA star has initially a radius of 640000000 m and a period of rotation about its axis of 20 days. Eventually it changes into a neutron star with a radius of only 50000 m and a period of 0.2 s. Assuming that the mass has not changed, find Assume a star has the shape of a sphere. (Suggestion: do it with formula first, then put the numbers in) [Recommended time : 5-8 minutes] (a) the ratio of initial to final angular momentum (Li/Lf) Oa. 1.42E+15 Ob. 19 Oc. 0.0527 Od. 7.06E-16 (b) the ratio of initial to final kinetic energy Oa. 8.18E-23 Ob. 456000 Oc. 2.19E-6 Od. 1.22E+22 52%arrow_forwardWhen the Sun becomes a red giant, it's luminosity will be 2000 times its current value. The solar flux at Earth will also increase by a factor of 2000. Neglecting the greenhouse effect, the surface temperature of the earth is determined by thermal equilibrium: the flux of radiation absorbed equals the flux of radiation emitted. This means the Earth's surface flux must also increase by a factor of 2000. If the current average surface temperature is 58 degrees F, what will the average surface temperature be when the Sun is a red giant. Express your answer in units of degrees Fahrenheit. [Hint: Recall that the Stefan-Boltzmann law says that the flux F emitted by a blackbody is related to its surface temperature T (measured in Kelvins) is F=σT4 . Use this law in the form of a ratio, expressing T in Kelvins. Then convert back to Fahrenheit.]arrow_forward
- We learned in class that, when stars collapse under their own gravity, they conserve angular momentum, which is proportional to mass times radius times rotational speed. Suppose the entire sun (radius 695,700 km) were to collapse to a neutron star with a radius of only 10 km. Before the collapse, the rotational speed at the equator = 2.0 km/s, and the rotational period is 25 days. Using the same steps that you used for the white dwarf calculations, calculate the final rotation period if the entire sun were to collapse to a 10 km radius neutron star. Give your answer in units of seconds. Answer: Checkarrow_forwardIn SN1987a the neutrino signal arrived about 3 hours before the optical signal. This suggests that it took 3 hours for the shockwave to propagate out through the star. If the blue supergiant progenitor to SN1987a had a radius of 10 ?⊙ R ⊙ , and assuming the shockwave was spherical and propagated from the center of the star, estimate the speed of the shockwave in km/s.arrow_forwardA main sequence star of mass 25 M⊙has a luminosity of approximately 80,000 L⊙. a. At what rate DOES MASS VANISH as H is fused to He in the star’s core? Note: When we say “mass vanish '' what we really mean is “gets converted into energy and leaves the star as light”. Note: approximate answer: 3.55 E14 kg/s b. At what rate is H converted into He? To do this you need to take into account that for every kg of hydrogen burned, only 0.7% gets converted into energy while the rest turns into helium. Approximate answer = 5E16 kg/s c. Assuming that only the 10% of the star’s mass in the central regions will get hot enough for fusion, calculate the main sequence lifetime of the star. Put your answer in years, and compare it to the lifetime of the Sun. It should be much, much shorter. Approximate answer: 30 million years.arrow_forward
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