Universe: Stars And Galaxies
Universe: Stars And Galaxies
6th Edition
ISBN: 9781319115098
Author: Roger Freedman, Robert Geller, William J. Kaufmann
Publisher: W. H. Freeman
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Chapter 24, Problem 23Q
To determine

(a)

Whether the aliens living in our Milky Way Galaxy will see the emission dominated by the jet.

To determine

(b)

Whether the aliens living in other Galaxy will see the emission dominated by the jet.

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For each problem, use the following values: c = 3x108 m/s mass of the sun = 1.989 x 1030 kg luminosity of the sun = 3.828 x 1026 W 1 AU = 1.496 x 1011 m 1 pc = 3.262 light years = 3.086 x 1016 m 1 year=3.154x107 seconds Critical density of our Universe (expressed as a mass density): Pcrit =8.7 x 10.27 kg m-³ Critical energy density of our Universe: Ecrit = Pcrit c² G=6.674 × 10-11 m³.kg-1.s-2 1 eV = 1.60218 x10-19. Boltzmann constant: kg = 1.381 x 10-23 JK-18.617 × 10-5 eV K-1 energy density constant (in Stefan Boltzmann Law): a = 7.566 x 10-16 Jm-3 K-4 -4.7 x 10-³ MeV m-3 K-4 Constant in Wein displacement law: b = 2.898 x 10-3 m K baryon-to-photon ratio, n= 6 x 10-10
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Another commonly calculated velocity in galactic dynamics is the escape velocity vesc, that is the minimum velocity a star must have in order to escape the gravitational field of the galaxy. (a) Starting from the work required to move a body over a distance dr against f show that the escape velocity from a point mass galaxy is vse = 2GM/r where r is your initial distance. (b) Since we know galaxies aren't actually point-masses, also show that vesc from r for a galaxy with a p(r) x r-² density profile is vse = 2v²(1+ ln(R/r)). Here you must assume that R is a cutoff radius at which the mass density is zero. (c) The largest velocity measured for any star in the solar neighbourhood, at r=8 kpc, is 440 km/s. Assuming that this star is still bound to the galaxy, find the lower limit (in kiloparsecs), to the cutoff radius R and a lower limit (in solar units) to the mass of the galaxy. Note the solar rotation velocity is 220 km/s.
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