Cosmic Perspective Fundamentals
3rd Edition
ISBN: 9780134988504
Author: Bennett, Jeffrey O., Donahue, M. (megan), SCHNEIDER, Nicholas, Voit, Mark
Publisher: Pearson,
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Textbook Question
Chapter 10, Problem 3QQ
Choose the best answer to each of the following. Explain your reasoning.
Why does matter falling toward a white dwarf, neutron star, black hole in a binary system form an accertion disk? (a) because the central objects spins very rapidly (b) because the infalling matter has some
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Students have asked these similar questions
Using MBH
=
6.6 × 10 Mo, calculate the below.
a. Find radius of the Schwarzschild sphere (Schwarzschild radius Rs). You
can calculated from the appropriate formula or just use the fact that for
an object of 1 solar mass Rs = 3 km.
b. Express Rs in km, in AU, in parsecs.
c. Using the distance to M87 and your result above, find angular radius of
the SMBH (Schwarzschild radius). Express it in arcseconds (") and micro-
arcseconds (pas)
d. Take the radius of Pluto's orbit equal to 40 AU and find its angular size
(in micro-arcseconds, pas) at the distance of M87.
Question B1
[This question will required roughly two single-sided A4 pages to answer.]
Consider a hypothetical, spherically symmetric star of mass M and radius R, for which the den-
sity profile is represented by p(r) = Pc [1 − (r/R)²], where pc is the central density and r is the
radial distance from the center of the star.
a) If the star is in hydrostatic equilibrium, by considering the forces acting on a volume ele-
ment, show that the following expression must apply:
dP
dr
Gm(r) p
12
where P is the pressure as a function of radial position and m(r) is the mass interior to the
radius r.
b) For the hypothetical star, with the given density as a function of radius p(r) = pc [1-(r/R)²],
show that m(r) can be written as
m(r) = 1½πr³ p
31.2
5R²
c) Show that the average density p of the star (i.e., total mass divided by total volume) is given
by p = 0.4pc.
d)
e)
Given that the pressure is zero when r = R, show that the central pressure is given by
Pe=
15 G M²
16π R4
ΜΗ
The star is…
Match each characteristic below to the appropriate stellar end state.
(Select W-White dwarf, N-Neutron star, B-Black hole. If the first is W and the rest N, enter
WNNNNNNN).
A) Has a mass no greater than 1.4 solar-masses.
B) Sometimes appears as a pulsar.
C) Size defined by its Schwarzschild radius.
D) In a binary system it can explode as a supernova.
E) Supported by electron degeneracy pressure.
F) Typically about the size of Earth.
G) Usually has a very strong magnetic field.
H) Viewed from afar, time stops at its event horizon.
Answer:
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Chapter 10 Solutions
Cosmic Perspective Fundamentals
Ch. 10 - Choose the best answer to each of the following....Ch. 10 - Choose the best answer to each of the following....Ch. 10 - Choose the best answer to each of the following....Ch. 10 - Choose the best answer to each of the following....Ch. 10 - Choose the best answer to each of the following....Ch. 10 - Prob. 6QQCh. 10 - Choose the best answer to each of the following....Ch. 10 - Choose the best answer to each of the following....Ch. 10 - Choose the best answer to each of the following....Ch. 10 - Choose the best answer to each of the following....
Ch. 10 - Choose the best answer to each of the following....Ch. 10 - Choose the best answer to each of the following....Ch. 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...Ch. 10 - Explain all answers clearly, with complete...Ch. 10 - Prob. 22SEQ
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- Please do not give solution in image formate thanku Q: You’ve just discovered another new X-ray binary, which we will call Hyp-X2 (“Hyp” for hypothetical). The system Hyp-X2 contains a bright, G2 main-sequence star orbiting an unseen companion. The separation of the stars is estimated to be 12 million kilometers, and the orbital period of the visible star is 5 days. Use Newton’s version of Kepler’s third law to calculate the sum of the masses of the two stars in the system. a)Express your answer in kilograms to two significant figures. b) Give your answer from the previous part in solar masses. ( Msun= 2.0 x 10 /30 kg). Express your answer as a multiple of sun’s mass to two significant figures. C) Determine the mass of the unseen companion. ( Hint: A G2 main-sequence star has a mass of 1 Msun.) Express your answer as a multiple of sun’s mass to two significant figures. The previous answer was not correct, please help mearrow_forwardMatch each characteristic below to the appropriate stellar end state. (Select W-White dwarf, N-Neutron star, B-Black hole. If the first is W and the rest N, enter WNNNNNNN). A) Size defined by its Schwarzschild radius. B) Typically about the size of Earth. C) Usually has a very strong magnetic field. D) In a binary system it can explode as a supernova. E) Supported by electron degeneracy pressure. F) Sometimes appears as a pulsar. G) Viewed from afar, time stops at its event horizon. H) Has a mass no greater than 1.4 solar-masses.arrow_forwardPlease solve accurate and exact this is very importantarrow_forward
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