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 22, Problem 34Q
To determine

The comparison of the kind of spiral arms that is produced by the density waves with those produced by self propagating star formation.

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Use the following formula (fitted to data) M = -4x10-13n gR Mo/year for the mass loss of asymptotic giant branch stars to: a) explain why L, g (gravity on surface), and R enter the equation the way they do (nominator or denominator). b) show that the expression for M is equivalent to LR M = -4x10-13n Mo/year M c) estimate the mass loss rate of a star with M = 1 Mo, L = 7000 Lo, T = 3000 K. Assume n = 1 and use the Stefan-Boltzmann equation to calculate R (in Ro).
Assume that the umber density of stars in the Milky Way is 0.14 pc-3. There are 10" stars uniformly distributed across the galaxy. Also assume that there is one supernova every 30 years and all of them have same luminosity. Find the probablity, P, of a supernova causing extinction on Earth in total life span of the Sun.
A planetary nebula expanded in radius 0.3 arc seconds in 30 years.  Doppler measurements show the nebula is expanding at a rate of 35 km/s.  How far away is the nebula in parsecs? First, determine what distance the nebular expanded in parsecs during the time mentioned.  Δd = vpc/sTs So we first need to convert the rate into pc/s and the time into seconds: vpc/s = vkm/s (1 pc / 3.09 x 1013km) vpc/s = ? Ts = (Tyr)(365 days/yr)(24 hrs/day)(3600 s/hr) Ts = ? s Δd= vpc/sTs Therefore, Δd = ? pc
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